Author: "Le Brun V." / Topic: astrophysics::galaxy astrophysics - Searchworks@Jio Institute Digital Library Search Results

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116 results on '"Le Brun V."'

1. Estimating the galaxy two-point correlation function using a split random catalog

Author: Gargiulo, A., Cucciati, O., Garilli, B., Scodeggio, M., Bolzonella, M., Zamorani, G., De Lucia, G., Krywult, J., Guzzo, L., Granett, B. R., de la Torre, S., Abbas, U., Adami, C., Arnouts, S., Bottini, D., Cappi, A., Franzetti, P., Fritz, A., Haines, C., Hawken, A. J., Iovino, A., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Moutard, T., Polletta, M., Pollo, A., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Bel, J., Branchini, E., Coupon, J., Ilbert, O., Moscardini, L., Peacock, J. A., Gargiulo, A., Cucciati, O., Garilli, B., Scodeggio, M., Bolzonella, M., Zamorani, G., De Lucia, G., Krywult, J., Guzzo, L., Granett, B. R., de la Torre, S., Abbas, U., Adami, C., Arnouts, S., Bottini, D., Cappi, A., Franzetti, P., Fritz, A., Haines, C., Hawken, A. J., Iovino, A., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Moutard, T., Polletta, M., Pollo, A., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Bel, J., Branchini, E., Coupon, J., Ilbert, O., Moscardini, L., and Peacock, J. A.
Subjects: formation [galaxies], galaxies: evolution, galaxies: formation, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies]
Abstract: We use the unparalleled statistics of the VIPERS survey to investigate the relation between the surface mean stellar mass density Sigma = M/(2 pi R-e(2)) of massive passive galaxies (MPGs, M >= 10(11) M-circle dot) and their local environment in the redshift range 0.5 2 x 10(11) M-circle dot, we find an excess of MPGs with low Sigma and a deficit of high-Sigma MPGs in the densest regions with respect to other environments. We interpret this result as due to the migration of some high-Sigma MPGs (= 0.8 migrate to the MPG population. Here, we investigate the Sigma-delta relation of MSFGs at z >= 0.8 and find that it is consistent within 1 sigma with that of low-Sigma MPGs at z = 0.8 are consistent in terms of number and environment with being the progenitors of low-Sigma MPGs at z < 0.8.
Published: 2019

2. The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Author: Gargiulo, A., Cucciati, O., Garilli, B., Scodeggio, M., Bolzonella, M., Zamorani, G., De Lucia, G., Krywult, J., Guzzo, L., Granett, B. R., de la Torre, S., Abbas, U., Adami, C., Arnouts, S., Bottini, D., Cappi, A., Franzetti, P., Fritz, A., Haines, C., Hawken, A. J., Iovino, A., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Moutard, T., Polletta, M., Pollo, A., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Bel, J., Branchini, E., Coupon, J., Ilbert, O., Moscardini, L., Peacock, J. A., Gargiulo, A., Cucciati, O., Garilli, B., Scodeggio, M., Bolzonella, M., Zamorani, G., De Lucia, G., Krywult, J., Guzzo, L., Granett, B. R., de la Torre, S., Abbas, U., Adami, C., Arnouts, S., Bottini, D., Cappi, A., Franzetti, P., Fritz, A., Haines, C., Hawken, A. J., Iovino, A., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Moutard, T., Polletta, M., Pollo, A., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Bel, J., Branchini, E., Coupon, J., Ilbert, O., Moscardini, L., and Peacock, J. A.
Subjects: formation [galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies]
Abstract: We use the unparalleled statistics of the VIPERS survey to investigate the relation between the surface mean stellar mass density Sigma = M/(2 pi R-e(2)) of massive passive galaxies (MPGs, M >= 10(11) M-circle dot) and their local environment in the redshift range 0.5 2 x 10(11) M-circle dot, we find an excess of MPGs with low Sigma and a deficit of high-Sigma MPGs in the densest regions with respect to other environments. We interpret this result as due to the migration of some high-Sigma MPGs (= 0.8 migrate to the MPG population. Here, we investigate the Sigma-delta relation of MSFGs at z >= 0.8 and find that it is consistent within 1 sigma with that of low-Sigma MPGs at z = 0.8 are consistent in terms of number and environment with being the progenitors of low-Sigma MPGs at z < 0.8.
Published: 2019

3. 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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4. The VIMOS Public Extragalactic Redshift Survey

Author: Granett, B. R., Branchini, ENZO FRANCO, Guzzo, L., Abbas, U., Adami, C., Arnouts, S., Bel, J., Bolzonella, M., Bottini, D., Cappi, A., Coupon, J., Cucciati, O., Davidzon, I., De Lucia, G., de la Torre, S., Fritz, A., Franzetti, P., Fumana, M., Garilli, B., Ilbert, O., Iovino, A., Krywult, J., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Mccracken, H. J., Polletta, M., Pollo, A., Scodeggio, M., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Burden, A., Di Porto, C., Marchetti, A., Marinoni, C., Mellier, Y., Moutard, T., Moscardini, L., Nichol, R. C., Peacock, J. A., Percival, W. J., Zamorani, G., Granett, B. R., Branchini, ENZO FRANCO, Guzzo, L., Abbas, U., Adami, C., Arnouts, S., Bel, J., Bolzonella, M., Bottini, D., Cappi, A., Coupon, J., Cucciati, O., Davidzon, I., De Lucia, G., de la Torre, S., Fritz, A., Franzetti, P., Fumana, M., Garilli, B., Ilbert, O., Iovino, A., Krywult, J., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Mccracken, H. J., Polletta, M., Pollo, A., Scodeggio, M., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Burden, A., Di Porto, C., Marchetti, A., Marinoni, C., Mellier, Y., Moutard, T., Moscardini, L., Nichol, R. C., Peacock, J. A., Percival, W. J., and Zamorani, G.
Subjects: methods: statistical, large-scale structure of Universe, cosmology: observations, galaxies: statistics, cosmological parameters, methods: data analysis, observations, galaxies: statistics, cosmological parameters, methods: statistical, methods: data analysis [large-scale structure of Universe, cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Aims: Using the VIMOS Public Extragalactic Redshift Survey (VIPERS) we aim to jointly estimate the keyparameters that describe the galaxy density field and its spatial correlations in redshift space. Methods: We use the Bayesian formalism to jointly reconstruct the redshift-space galaxy density field, power spectrum, galaxy bias and galaxy luminosity function given the observations and survey selection function. The high-dimensional posterior distribution is explored using the Wiener filter within a Gibbs sampler. We validate the analysis using simulated catalogues and apply it to VIPERS data taking into consideration the inhomogeneous selection function. Results: We present joint constraints on the anisotropic power spectrum, and the bias and number density of red and blue galaxy classes in luminosity and redshift bins as well as the measurement covariances of these quantities. We find that the inferred galaxy bias and number density parameters are strongly correlated although they are only weakly correlated with the galaxy power spectrum. The power spectrum and redshift-space distortion parameters are in agreement with previous VIPERS results with the value of the growth rate fσ8 = 0.38 with 18% uncertainty at redshift 0.7.
Published: 2015

5. Measuring Large-Scale Structure atz∼ 1 with the VIPERS galaxy survey

Author: GUZZO, Luigi, Abbas, U., Adami, Christophe, Arnouts, Stephane, Bel, Julien, Bolzonella, M., Bottini, D., Branchini, Enzo Franco, Burden, Angela, Cappi, A., Coupon, Jean, Cucciati, O., Davidzon, Iary, de la Torre, Silvain, De Lucia, G., Di Porto, Cinzia, Franzetti, P., Fritz, Alexander, Fumana, M., GARILLI, BIANCA MARIA ROSA, Granett, B. R., Guennou, L., Hawken, A., Ilbert, O., Iovino, A., Krywult, J., Le Brun, V., Le Fevre, O., Maccagni, D., Malek, K., Marchetti, A., Marinoni, C., Marulli, F., McCracken, H. J., Mellier, Y., Moscardini, L., Nichol, R. C., Paioro, L., Peacock, J. A., Percival, W. J., Phleps, S., POLLETTA, MARIA DEL CARMEN, Pollo, A., Rota, S., Schlagenhaufer, H., SCODEGGIO, MARCO, Solarz, A., Tasca, L. A. M., Tojeiro, R., VERGANI, DANIELA, Wolk, M., Zamorani, G., and ZANICHELLI, Alessandra
Subjects: Physics, Space and Planetary Science, Scale structure, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy
Abstract: The VIMOS Public Extragalactic Redshift Survey (VIPERS) is the largest redshift survey ever conducted with the ESO telescopes. It has used the Very Large Telescope to collect nearly 100,000 redshifts from the general galaxy population at 0.5
Published: 2016

6. The evolving star formation rate: M-star relation and sSFR since z similar or equal to 5 from the VUDS spectroscopic survey

Author: Tasca, L. A. M., Le Fevre, O., Hathi, N. P., Schaerer, D., Ilbert, O., Zamorani, G., Lemaux, B. C., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Amorín, R., Bardelli, S., Cassara, L. P., Castellano, M., Cimatti, Alessandro, Cucciati, O., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Paltani, S., Ribeiro, B., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vergani, D., Capak, P., Charlot, S., Contini, T., Torre, S., Dunlop, J., Fotopoulou, S., Koekemoer, A., Lopez-Sanjuan, C., Mellier, Y., Pforr, J., Salvato, M., Scoville, N., Taniguchi, Y., Wang, P. W., 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 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), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Roma (OAR), Oncology Institute of Southern Switzerland, INAF - Osservatorio Astronomico di Bologna (OABO), University of Bologna/Università di Bologna, Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), INAF- Milano, INAF - Osservatorio Astrofisico di Arcetri (OAA), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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), SUPA, Institute for Astronomy, University of Edinburgh, Aristotle University of Thessaloniki, Space Telescope Science Institute (STSci), Institute of cosmology and gravitation, University of Portsmouth, Max-Planck-Institut für Extraterrestrische Physik (MPE), Excellence Cluster Universe, excellence cluster centre, California Institute of Technology (CALTECH), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Bologna, and University of Geneva [Switzerland]
Subjects: Galaxies: star formation, Galaxies: high-redshift, Galaxies: evolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: International audience; We study the evolution of the star formation rate (SFR) - stellar mass (M-star) relation and specific star formation rate (sSFR) of star-forming galaxies (SFGs) since a redshift z similar or equal to 5.5 using 2435 (4531) galaxies with highly reliable spectroscopic redshifts in the VIMOS Ultra-Deep Survey (VUDS). It is the first time that these relations can be followed over such a large redshift range from a single homogeneously selected sample of galaxies with spectroscopic redshifts. The log(SFR) - log(M-star) relation for SFGs remains roughly linear all the way up to z = 5, but the SFR steadily increases at fixed mass with increasing redshift. We find that for stellar masses M-star \textgreater= 3.2 x 10(9) M-circle dot the SFR increases by a factor of similar to 13 between z = 0.4 and z = 2.3. We extend this relation up to z = 5, finding an additional increase in SFR by a factor of 1.7 from z = 2.3 to z = 4.8 for masses M-star = 1010 M-circle dot. We observe a turn-off in the SFR-M-star relation at the highest mass end up to a redshift z similar to 3.5. We interpret this turn-off as the signature of a strong on-going quenching mechanism and rapid mass growth. The sSFR increases strongly up to z similar to 2, but it grows much less rapidly in 2 \textless z \textless 5. We find that the shape of the sSFR evolution is not well reproduced by cold gas accretion-driven models or the latest hydrodynamical models. Below z similar to 2 these models have a flatter evolution (1+z)(Phi) with Phi = 2-2.25 compared to the data which evolves more rapidly with Phi = 2.8 +/- 0.2. Above z similar to 2, the reverse is happening with the data evolving more slowly with Phi = 1.2 +/- 0.1. The observed sSFR evolution over a large redshift range 0 \textless z \textless 5 and our finding of a non-linear main sequence at high mass both indicate that the evolution of SFR and M-star is not solely driven by gas accretion. The results presented in this paper emphasize the need to invoke a more complex mix of physical processes including major and minor merging to further understand the co-evolution of the SFR and stellar mass growth.
Published: 2015
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7. Extreme emission-line galaxies out to z similar to 1 in zCOSMOS I. Sample and characterization of global properties

Author: Amorin, R., Perez-Montero, F., Contini, T., Vilchez, J. M., Bolzonella, M., Tasca, L. A. M., Lamareille, F., Zamorani, G., Maier, C., Carollo, C. M., Kneib, J. -P., Le Fevre, O., Lilly, S., Mainieri, V., Renzinis, A., Scodeggio, M., Bardelli, S., Bongiorno, A., Caputi, K., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Kovac, K., Le Borgne, J. -F., Le Brun, V., Mignoli, M., Pello, R., Peng, Y., Presotto, V., Ricciardelli, E., Silverman, J. D., Tanaka, M., Tresse, L., Vergani, D., Zucca, E., and Kapteyn Astronomical Institute
Subjects: ACTIVE GALACTIC NUCLEI, galaxies: irregular galaxies: star formation, ULTRA DEEP FIELD, METAL-POOR GALAXIES, galaxies: fundamental parameters, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, LYMAN BREAK GALAXIES, LY-ALPHA EMITTERS, LUMINOSITY-METALLICITY RELATION, COMPACT DWARF GALAXIES, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, DIGITAL SKY SURVEY, galaxies: abundances, Astrophysics::Earth and Planetary Astrophysics, GREEN PEA GALAXIES, galaxies: evolution, Astrophysics::Galaxy Astrophysics
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 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 "direct" and "strong-line" methods. Results. The EELGs are extremely compact (r(50) similar to 1.3 kpc), low-mass (M-* similar to 10(7)-10(10) M-circle dot) galaxies forming stars at unusually high specific star formation rates (sSFR equivalent to SFR/M-star 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 Ly alpha 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 Z(circle dot)) including a handful of extremely metal-deficient ( 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.
Published: 2015

8. Extreme emission-line galaxies out to z similar to 1 in zCOSMOS I. Sample and characterization of global properties

Author: Amorín, R., Perez-Montero, F., Contini, T., Vílchez, J. M., Bolzonella, M., Tasca, L. A. M., Lamareille, F., Zamorani, G., Maier, C., Carollo, C. M., Kneib, J. -P., Le Fevre, O., Lilly, S., Mainieri, V., Renzini, A., Scodeggio, M., Bardelli, S., Bongiorno, A., Caputi, K., Cucciati, O., Torre, S., Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Knobel, C., Kovac, K., Le Borgne, J. -F., Le Brun, V., Mignoli, M., Pello, R., Peng, Y., Presotto, V., Ricciardelli, E., Silverman, J. D., Tanaka, M., Tresse, L., Vergani, D., Zucca, E., INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), 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 Vienna [Vienna], University of Chicago, Ecole Polytechnique Fédérale de Lausanne (EPFL), European Southern Observatory (ESO), INAF- Milano, INAF - Osservatorio Astronomico di Bologna (OABO), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], Hunan Normal University (HNU), Università degli studi di Trieste = University of Trieste, INAF - Osservatorio Astronomico di Trieste (OAT), INAF - Osservatorio Astrofisico di Arcetri (OAA), Oncology Institute of Southern Switzerland, European Project: 312725,EC:FP7:SPA,FP7-SPACE-2012-1,ASTRODEEP(2013), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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), Hunan Normal University, and Università degli studi di Trieste
Subjects: Galaxies: fundamental parameters, Galaxies: star formation, Galaxies: abundances, Astrophysics::Solar and Stellar Astrophysics, Galaxies: evolution, Galaxies: irregular, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: starburst, Astrophysics::Galaxy Astrophysics
Abstract: International audience; 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 \textless= z \textless= 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 “direct” and “strong-line” methods. Results. The EELGs are extremely compact (r(50) similar to 1.3 kpc), low-mass (M-* similar to 10(7)-10(10) M-circle dot) galaxies forming stars at unusually high specific star formation rates (sSFR equivalent to SFR/M-star 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 Ly alpha 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 Z(circle dot)) including a handful of extremely metal-deficient (\textless0.1 Z(circle dot)) EELGs. While similar to 80% of the EELGs show non-axisymmetric morphologies, including clumpy and cometary or tadpole galaxies, we find that similar to 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.
Published: 2015
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9. Stellar mass to halo mass relation from galaxy clustering in VUDS: a high star formation efficiency at z similar or equal to 3

Author: Durkalec, A., Le Fevre, O., Torre, S., Pollo, A., Cassata, P., Garilli, B., Le Brun, V., Lemaux, B. C., Maccagni, D., Pentericci, L., Tasca, L. A. M., Thomas, R., Vanzella, E., Zamorani, G., Zucca, E., Amorín, R., Bardelli, S., Cassara, L. P., Castellano, M., Cimatti, Alessandro, Cucciati, O., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N. P., Ilbert, O., Paltani, S., Ribeiro, B., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vereani, D., Capak, P., Charlot, S., Contini, T., Cuby, J. G., Dunlop, J., Fotopoulou, S., Koekemoer, A., Lopez-Sanjuan, C., Mellier, Y., Pforr, J., Salvato, M., Scoville, N., Taniguchi, Y., Wang, P. W., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Oncology Institute of Southern Switzerland, INAF - Osservatorio Astronomico di Bologna (OABO), University of Bologna/Università di Bologna, Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF- Milano, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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), SUPA, Institute for Astronomy, University of Edinburgh, Aristotle University of Thessaloniki, Space Telescope Science Institute (STSci), Max-Planck-Institut für Extraterrestrische Physik (MPE), Excellence Cluster Universe, excellence cluster centre, California Institute of Technology (CALTECH), ANR-11-IDEX-0001,Amidex,INITIATIVE D'EXCELLENCE AIX MARSEILLE UNIVERSITE(2011), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), University of Bologna, University of Geneva [Switzerland], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and 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)
Subjects: Large-scale structure of Universe, Astrophysics::Solar and Stellar Astrophysics, Galaxies: evolution, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Early Universe, Astrophysics::Galaxy Astrophysics, Methods: statistical
Abstract: International audience; The relation between the galaxy stellar mass M-star and the dark matter halo mass M-h gives important information on the efficiency in forming stars and assembling stellar mass in galaxies. We present measurements of the ratio of stellar mass to halo mass (SMHR) at redshifts 2 \textless z \textless 5, obtained from the VIMOS Ultra Deep Survey. We use halo occupation distribution (HOD) modelling of clustering measurements on similar to 3000 galaxies with spectroscopic redshifts to derive the dark matter halo mass M-h, and spectral energy density fitting over a large set of multi-wavelength data to derive the stellar mass M-star and compute the SMHR = M-star/M-h. We find that the SMHR ranges from 1% to 2.5% for galaxies with M-star = 1.3 x 10(9) M-star to M-star = 7.4 x 10(9) M-circle dot in DM halos with M-h = 1.3 x 10(11) M-circle dot to M-h = 3 x 10(11) M-circle dot. We derive the integrated star formation efficiency (ISFE) of these galaxies and find that the star formation efficiency is a moderate 6-9% for lower mass galaxies, while it is relatively high at 16% for galaxies with the median stellar mass of the sample similar to 7 x 10(9) M-circle dot. The lower ISFE at lower masses may indicate that some efficient means of suppressing star formation is at work (like SNe feedback), while the high ISFE for the average galaxy at z similar to 3 indicates that these galaxies efficiently build up their stellar mass at a key epoch in the mass assembly process. Based on our results, we propose a possible scenario in which the average massive galaxy at z similar to 3 begins to experience truncation of its star formation within a few million years.
Published: 2015
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10. The Nonlinear Biasing of the zCOSMOS Galaxies up to z ~ 1 from the 10k Sample

Author: Kova, #269, Porciani C., Lilly S. J., Marinoni C., Guzzo L., Zamorani G., Iovino A., Oesch P., Bolzonella M., Peng Y., Meneux B., Zucca E., Bardelli S., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Finoguenov A., Franzetti P., Garilli B., Kampczyk P., Knobel C., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pello R., Perez Montero E., Pozzetti L., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., Abbas U., Bottini D., Cappi A., Cassata P., Fumana M., Koekemoer A. M., Leauthaud A., Maccagni D., McCracken H. J., Memeo P., Scaramella R., Scoville N. Z., CUCCIATI, OLGA, CIMATTI, ANDREA, Kova&#269, K., Porciani C., Lilly S. J., Marinoni C., Guzzo L., Cucciati O., Zamorani G., Iovino A., Oesch P., Bolzonella M., Peng Y., Meneux B., Zucca E., Bardelli S., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Finoguenov A., Franzetti P., Garilli B., Kampczyk P., Knobel C., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Perez-Montero E., Pozzetti L., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Koekemoer A. M., Leauthaud A., Maccagni D., McCracken H. J., Memeo P., Scaramella R., and Scoville N. Z.
Subjects: Physics, cosmology: observation, Field (physics), 010308 nuclear & particles physics, Dark matter, Astronomy and Astrophysics, Biasing, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, Space and Planetary Science, cosmology: observations, 0103 physical sciences, Halo effect, galaxies: evolution, galaxies: statistics, 010303 astronomy & astrophysics, Smoothing, Astrophysics::Galaxy Astrophysics
Abstract: We use the zCOSMOS galaxy overdensity field to study the biasing of galaxies in the COSMOS field. By comparing the probability distribution function of the galaxy density contrast δ g to the lognormal approximation of the mass density contrast δ, we obtain the mean biasing function b(δ, z, R) between the galaxy and matter overdensity fields and its second moments \hat{b} and \tilde{b}. Over the redshift interval 0.4 < z < 1 the conditional mean function langδ g |δrang = b(δ, z, R)δ is of a characteristic shape, requiring nonlinear biasing in the most overdense and underdense regions. Taking into account the uncertainties due to cosmic variance, we do not detect any significant evolution in the langδ g |δrang function, but we do detect a significant redshift evolution in the linear biasing parameter \hat{b} from 1.23 ± 0.11 at z ~ 0.55 to 1.62 ± 0.14 at z ~ 0.75, for a luminosity-complete sample of MB < -20 - z galaxies. The \hat{b} parameter does not change significantly with smoothing scale between 8 and 12 h -1 Mpc, but increases systematically with luminosity (at 2σ-3σ significance between the MB < -20.5 - z and MB < -20 - z samples). The nonlinearity parameter \tilde{b}/ \hat{b} is offset from unity by at most 2%, with an uncertainty of the same order. The \tilde{b}/\hat{b} parameter does not show any significant redshift evolution, dependence on the smoothing scale or on the luminosity. By matching the linear bias of galaxies to the halo bias, we infer that the MB < -20 - z galaxies reside in dark matter halos with a characteristic mass of about (2.6 - 5.6) × 1012 M sun with a small dependence on the adopted bias-mass relation. Our detailed error analysis and comparison with previous studies lead us to conclude that cosmic variance is the main contributor to the differences in the linear bias measured from different surveys. While our results support the general picture of biased galaxy formation up to z ~ 1, the fine-tuning of the galaxy formation models is still limited by the restrictions of the current spectroscopic surveys at these redshifts.
Published: 2011

11. The zCOSMOS-Bright survey: the clustering of early and late galaxy morphological types since z≃ 1

Author: de la Torre S., Le Fèvre O., Porciani C., Guzzo L., Meneux B., Abbas U., Tasca L., Carollo C. M., Contini T., Kneib J. P., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de Ravel L., Franzetti P., Garilli B., Halliday C., Iovino A., Kampczyk P., Knobel C., Koekemoer A. M., Kova, #269, Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J., Tanaka M., Tresse L., Vergani D., Zucca E., Bottini D., Cappi A., Cassata P., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Oesch P., Pozzetti L., Scaramella R., CUCCIATI, OLGA, CIMATTI, ANDREA, de la Torre S., Le Fèvre O., Porciani C., Guzzo L., Meneux B., Abbas U., Tasca L., Carollo C. M., Contini T., Kneib J.-P., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., Cucciati O., de Ravel L., Franzetti P., Garilli B., Halliday C., Iovino A., Kampczyk P., Knobel C., Koekemoer A. M., Kova&#269, K., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J., Tanaka M., Tresse L., Vergani D., Zucca E., Bottini D., Cappi A., Cassata P., Cimatti A., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Oesch P., Pozzetti L., and Scaramella R.
Subjects: cosmology: observation, galaxies: high-redshift, galaxies: statistic, Astrophysics::Cosmology and Extragalactic Astrophysics, large-scale structure of Universe, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: We measure the spatial clustering of galaxies as a function of their morphological type at z≃ 0.8, for the first time in a deep redshift survey with full morphological information. This is obtained by combining high-resolution Hubble Space Telescope imaging and Very Large Telescope spectroscopy for about 8500 galaxies to ? with accurate spectroscopic redshifts from the zCOSMOS-Bright redshift survey. At this epoch, early-type galaxies already show a significantly stronger clustering than late-type galaxies on all probed scales. A comparison to the Sloan Digital Sky Survey Data at z≃ 0.1 shows that the relative clustering strength between early and late morphological classes tends to increase with cosmic time at small separations, while on large scales it shows no significant evolution since z≃ 0.8. This suggests that most early-type galaxies had already formed in intermediate and dense environments at this epoch. Our results are consistent with a picture in which the relative clustering of different morphological types between z≃ 1 and 0 reflects the evolving role of environment in the morphological transformation of galaxies, on top of a global evolution driven by mass.
Published: 2011

12. The evolution of quiescent galaxies at high redshifts (z≥ 1.4)

Author: Domínguez Sánchez H., Gruppioni C., Ilbert O., Pozzetti L., McCracken H., Capak P., Le Floch E., Salvato M., Zamorani G., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Kova, #269, Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., Zucca E., POZZI, FRANCESCA, CIMATTI, ANDREA, CUCCIATI, OLGA, Domínguez Sánchez H., Pozzi F., Gruppioni C., Cimatti A., Ilbert O., Pozzetti L., McCracken H., Capak P., Le Floch E., Salvato M., Zamorani G., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., 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., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pelló R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tasca L. A. M., Tresse L., Vergani D., and Zucca E.
Subjects: galaxies: high-redshift, galaxies: star formation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: The goal of this work is to study the evolution of high-redshift (z≥ 1.4) quiescent galaxies over an effective area of ˜1.7 deg2 in the COSMOS field. Galaxies have been divided according to their star formation activity and the evolution of the different populations, in particular of the quiescent galaxies, has been investigated in detail. We have studied an IRAC (mag 3.6 μm < 22.0) selected sample of ˜18 000 galaxies at z≥ 1.4 in the COSMOS field with multiwavelength coverage extending from the U band to the Spitzer 24 μm one. We have derived accurate photometric redshifts (?) through a SED-fitting procedure. Other important physical parameters [masses, ages and star formation rates (SFR)] of the galaxies have been obtained using Maraston models. We have divided our sample into actively star-forming, intermediate and quiescent galaxies depending on their specific star formation rate (SSFR = SFR/M). We have computed the galaxy stellar mass function (GSMF) of the total sample and the different populations at z= 1.4-3.0. We have studied the properties of high-redshift quiescent galaxies finding that they are old (1-4 Gyr), massive (˜ 1010.65 M⊙), weakly star-forming stellar populations with low dust extinction [E(B-V) ≤ 0.15] and small e-folding time-scales (τ˜ 0.1-0.3 Gyr). We observe a significant evolution of the quiescent stellar mass function from 2.5 < z < 3.0 to 1.4 < z < 1.6, increasing by ˜1 dex in this redshift interval. We find that z˜ 1.5 is an epoch of transition of the GSMF: while the GSMF at z≳ 1.5 is dominated by the star-forming galaxies at all stellar masses, at z≲ 1.5 the contribution to the total GSMF of the quiescent galaxies is significant and becomes higher than that of the star-forming population for M≥ 1010.75 M⊙. The fraction of star-forming galaxies decreases from 60-20 per cent from z˜ 2.5-3.0 to 1.4-1.6 for M˜ 1011.0 M⊙, while the quiescent population increases from 10-50 per cent at the same redshift and mass intervals. We compare the fraction of quiescent galaxies derived with that predicted by theoretical models and find that the Kitzbichler & White model, implemented on the Millennium Simulation, is the one that better reproduces the shape of the data. Finally, we calculate the stellar mass density of the star-forming and quiescent populations as a function of redshift and find that there is already a significant number of quiescent galaxies at z > 2.5 (logρ[M⊙ Mpc-3]˜ 6), meaning that efficient star formation had to take place before that time.
Published: 2011

13. The bimodality of the 10k zCOSMOS-bright galaxies up to z ~ 1: a new statistical and portable classification based on the optical galaxy properties

Author: Coppa G., Mignoli M., Zamorani G., Bardelli S., Lilly S. J., Bolzonella M., Scodeggio M., Vergani D., Nair P., Pozzetti L., Zucca E., Carollo C. M., Contini T., Le Fèvre O., Renzini A., Mainieri V., Bongiorno A., Caputi K. I., de la Torre S., de Ravel L., Franzetti P., Garilli B., Memeo P., Iovino A., Kampczyk P., Kneib J. P., Knobel C., Koekemoer A. M., Kova, #269, Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Pellò R., Peng Y., Perez Montero E., Ricciardelli E., Scarlata C., Silverman J. D., Tanaka M., Tasca L., Tresse L., Abbas U., Bottini D., Capak P., Cappi A., Cassata P., Fumana M., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., Meneux B., Oesch P., Porciani C., Scaramella R., Scoville N., CIMATTI, ANDREA, CUCCIATI, OLGA, Coppa G., Mignoli M., Zamorani G., Bardelli S., Lilly S. J., Bolzonella M., Scodeggio M., Vergani D., Nair P., Pozzetti L., Cimatti A., Zucca E., Carollo C. M., Contini T., Le Fèvre O., Renzini A., Mainieri V., Bongiorno A., Caputi K. I., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Memeo P., Iovino A., Kampczyk P., Kneib J.-P., Knobel C., Koekemoer A. M., Kova&#269, K., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Pellò R., Peng Y., Perez-Montero E., Ricciardelli E., Scarlata C., Silverman J. D., Tanaka M., Tasca L., Tresse L., Abbas U., Bottini D., Capak P., Cappi A., Cassata P., Fumana M., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., Meneux B., Oesch P., Porciani C., Scaramella R., Scoville N., Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), University of Chicago, 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), 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), European Southern Observatory (ESO), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], AUTRES, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Ecole Polytechnique Fédérale de Lausanne (EPFL), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Département Informatique pour les Systèmes Coopératifs Ouverts et Décentralisés (ISCOD-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Institut Henri Fayol, Laboratoire Léon Brillouin (LLB - UMR 12), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Hunan Normal University, Spitzer Science Center, California Institute of Technology (CALTECH), 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), 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, Astronomy, 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), 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), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Hunan Normal University (HNU), 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), and Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, STAR-FORMATION, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], MORPHOLOGICAL CLASSIFICATION, 0103 physical sciences, Range (statistics), PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: general, Astronomy and Astrophysics, Space and Planetary Science, DIGITAL-SKY-SURVEY, 010308 nuclear & particles physics, FORMATION HISTORIES, HUBBLE DEEP FIELD, Order (ring theory), galaxies: fundamental parameters, ENVIRONMENTAL DEPENDENCE, Redshift survey, galaxies: general, Redshift, Galaxy, Bimodality, LUMINOSITY FUNCTION, SPECTROSCOPIC SAMPLE, STELLAR MASS FUNCTION, Cube, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Our goal is to develop a new and reliable statistical method to classify galaxies from large surveys. We probe the reliability of the method by comparing it with a three-dimensional classification cube, using the same set of spectral, photometric and morphological parameters.We applied two different methods of classification to a sample of galaxies extracted from the zCOSMOS redshift survey, in the redshift range 0.5 < z < 1.3. The first method is the combination of three independent classification schemes, while the second method exploits an entirely new approach based on statistical analyses like Principal Component Analysis (PCA) and Unsupervised Fuzzy Partition (UFP) clustering method. The PCA+UFP method has been applied also to a lower redshift sample (z < 0.5), exploiting the same set of data but the spectral ones, replaced by the equivalent width of H$��$. The comparison between the two methods shows fairly good agreement on the definition on the two main clusters, the early-type and the late-type galaxies ones. Our PCA-UFP method of classification is robust, flexible and capable of identifying the two main populations of galaxies as well as the intermediate population. The intermediate galaxy population shows many of the properties of the green valley galaxies, and constitutes a more coherent and homogeneous population. The fairly large redshift range of the studied sample allows us to behold the downsizing effect: galaxies with masses of the order of $3\cdot 10^{10}$ Msun mainly are found in transition from the late type to the early type group at $z>0.5$, while galaxies with lower masses - of the order of $10^{10}$ Msun - are in transition at later epochs; galaxies with $M 5\cdot 10^{10}$ Msun) mostly completed their transition before $z\sim 1$., 16 pages, 14 figures, accepted for publication in A&A
Published: 2010
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14. The VIMOS-VLT Deep Survey: evolution in the halo occupation number since z ~ 1

Author: Abbas, U., Torre, S., Le Fèvre, O., Guzzo, L., Marinoni, C., Meneux, B., Pollo, A., Zamorani, G., Bottini, D., Garilli, B., Le Brun, V., Maccagni, D., Scaramella, R., Scodeggio, M., Tresse, L., Vettolani, G., Zanichelli, A., Adami, C., Arnouts, S., Bardelli, S., Bolzonella, M., Cappi, A., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Gavignaud, I., Ilbert, O., Iovino, A., Lamareille, F., Mccracken, H.~j., Marano, B., Mazure, A., Merighi, R., Paltani, S., Pellò, R., Pozzetti, L., Radovich, M., Vergani, D., Zucca, E., Bondi, M., Bongiorno, A., Brinchmann, J., Cucciati, O., Ravel, L., Gregorini, L., Perez-Montero, E., Mellier, Y., Merluzzi, P., 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), Abbas U., de la Torre S., Le Fèvre O., Guzzo L., Marinoni C., Meneux B., Pollo A., Zamorani G., Bottini D., Garilli B., and Le brun V., Maccagni D., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Iovini A., Lamareille F., McCracken H.J., Marano B., Mazure A., Merighi R., Paltani S., Pello' R., Pozzetti L., Radovich M., Vergani D., Zucca E., Bondi M., Bongiorno A., Brinchmann ., Cucciati P., de Ravel L., Gregorini L., Perez-Montero E., Mellier Y., Merluzzi P.
Subjects: methods: statistical, surveys, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], galaxies: high-redshift, [INFO]Computer Science [cs], Astrophysics::Cosmology and Extragalactic Astrophysics, LARGE-SCALE STRUCTURE OF NIVERSE, large-scale structure of Universe, GALAXIES:HIGH-REDSHIFT, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, METHOD: STATISTICAL
Abstract: We model the evolution of the mean galaxy occupation of dark matter haloes over the range 0.1 < z < 1.3, using the data from the VIMOS-VLT Deep Survey. The galaxy projected correlation function wp(rp) was computed for a set of luminosity-limited subsamples and fits to its shape were obtained using two variants of halo occupation distribution (HOD) models. These provide us with a set of best-fitting parameters, from which we obtain the average mass of a halo and average number of galaxies per halo. We find that after accounting for the evolution in luminosity and assuming that we are largely following the same population, the underlying dark matter halo shows a growth in mass with decreasing redshift as expected in a hierarchical structure formation scenario. Using two different HOD models, we see that the halo mass grows by 90 per cent over the redshift interval z = [0.5, 1.0]. This is the first time the evolution in halo mass at high redshifts has been obtained from a single data survey and it follows the simple form seen in N-body simulations with M(z) = M0 e-βz, and β = 1.3 +/- 0.30. This provides evidence for a rapid accretion phase of massive haloes having a present-day mass M0 ~ 1013.5 h-1 Msolar, with a m > 0.1 M0 merger event occurring between redshifts of 0.5 and 1.0. Furthermore, we find that more luminous galaxies are found to occupy more massive haloes irrespective of the redshift. Finally, the average number of galaxies per halo shows little increase from redshift z ~ 1.0 to ~0.5, with a sharp increase by a factor of ~3 from z ~ 0.5 to ~0.1, likely due to the dynamical friction of subhaloes within their host haloes. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, program 070.A-9007(A), and on data obtained at the Canada-France-Hawaii Telescope, operated by the CNRS of France, CNRC in Canada and the University of Hawaii.
Published: 2010
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15. The XMM-Newton Wide-Field Survey in the COSMOS field (XMM-COSMOS): demography and multiwavelength properties of obscured and unobscured luminous AGN

Author: BRUSA, MARCELLA, LUSSO, ELISABETA, VIGNALI, CRISTIAN, Civano F., Comastri A., Miyaji T., Salvato M., Zamorani G., Cappelluti N., Fiore F., Hasinger G., Mainieri V., Merloni A., Bongiorno A., Capak P., Elvis M., Gilli R., Hao H., Jahnke K., Koekemoer A. M., Ilbert O., Le Floc'h E., Mignoli M., Schinnerer E., Silverman J. D., Treister E., Trump J. D., Zamojski M., Aldcroft T., Aussel H., Bardelli S., Bolzonella M., Cappi A., Caputi K., Contini T., Finoguenov A., Fruscione A., Garilli B., Impey C. D., Iovino A., Iwasawa K., Kampczyk P., Kartaltepe J., Kneib J. P., Knobel C., Kovac K., Lamareille F., Leborgne J. F., Le Brun V., Le Fevre O., Lilly S. J., Maier C., McCracken H. J., Pello R., Peng Y. J, Perez Montero E., de Ravel L., Sanders D., Scodeggio M., Scoville N. Z., Tanaka M., Taniguchi Y., Tasca L., de la Torre S., Tresse L., Vergani D., Zucca E., Brusa M., Civano F., Comastri A., Miyaji T., Salvato M., Zamorani G., Cappelluti N., Fiore F., Hasinger G., Mainieri V., Merloni A., Bongiorno A., Capak P., Elvis M., Gilli R., Hao H., Jahnke K., Koekemoer A. M., Ilbert O., Le Floc'h E., Lusso E., Mignoli M., Schinnerer E., Silverman J. D., Treister E., Trump J. D., Vignali C., Zamojski M., Aldcroft T., Aussel H., Bardelli S., Bolzonella M., Cappi A., Caputi K., Contini T., Finoguenov A., Fruscione A., Garilli B., Impey C. D., Iovino A., Iwasawa K., Kampczyk P., Kartaltepe J., Kneib J. P., Knobel C., Kovac K., Lamareille F., Leborgne J.-F., Le Brun V., Le Fevre O., Lilly S. J., Maier C., McCracken H. J., Pello R., Peng Y-J, Perez-Montero E., de Ravel L., Sanders D., Scodeggio M., Scoville N. Z., Tanaka M., Taniguchi Y., Tasca L., de la Torre S., Tresse L., Vergani D., and Zucca E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active – surveys – X-rays: diffuse background – X-rays: galaxies – X-rays: general, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the final optical identifications of the medium-depth (~60 ksec), contiguous (2 deg^2) XMM-Newton survey of the COSMOS field. XMM-Newton has detected ~800 X-ray sources down to limiting fluxes of ~5x10^{-16}, ~3x10^{-15}, and ~7x10^{-15} erg/cm2/s in the 0.5-2 keV, 2-10 keV and 5-10 keV bands, respectively. The work is complemented by an extensive collection of multi-wavelength data from 24 micron to UV, available from the COSMOS survey, for each of the X-ray sources, including spectroscopic redshifts for ~50% of the sample, and high-quality photometric redshifts for the rest. The XMM and multiwavelength flux limits are well matched: 1760 (98%) of the X-ray sources have optical counterparts, 1711 (~95%) have IRAC counterparts, and 1394 (~78%) have MIPS 24micron detections. Thanks to the redshift completeness (almost 100%) we were able to constrain the high-luminosity tail of the X-ray luminosity function confirming that the peak of the number density of logL_X>44.5 AGN is at z~2. Spectroscopically-identified obscured and unobscured AGN, as well as normal and starforming galaxies, present well-defined optical and infrared properties. We devised a robust method to identify a sample of ~150 high redshift (z>1), obscured AGN candidates for which optical spectroscopy is not available. We were able to determine that the fraction of the obscured AGN population at the highest (L_X>10^{44} erg s^{-1}) X-ray luminosity is ~15-30% when selection effects are taken into account, providing an important observational constraint for X-ray background synthesis. We studied in detail the optical spectrum and the overall spectral energy distribution of a prototypical Type 2 QSO, caught in a stage transitioning from being starburst dominated to AGN dominated, which was possible to isolate only thanks to the combination of X-ray and infrared observations., ApJ, in press. 59 pages, 14 figures, 2 Tables. A few typos corrected and a reference added. Table 2 is also available at http://www.mpe.mpg.de/XMMCosmos/xmm53_release ; a version of the paper in ApJ format (27 pages) is available at http://www.mpe.mpg.de/XMMCosmos/xmm53_release/brusa_xmmcosmos_optid.pdf
Published: 2010
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16. The [O iii] emission line luminosity function of optically selected type-2 AGN from zCOSMOS

Author: Bongiorno A., Mignoli M., Zamorani G., Lamareille F., LANZUISI, GIORGIO, Miyaji T., Bolzonella M., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Caputi K., Civano F., Coppa G., de La Torre S., de Ravel L., Franzetti P., Garilli B., Halliday C., Hasinger G., Koekemoer A. M., Iovino A., Kampczyk P., Knobel C., Kova, #269, Le Borgne J. F., Le Brun V., Maier C., Merloni A., Nair P., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Salvato M., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Scaramella R., BRUSA, MARCELLA, CUCCIATI, OLGA, CIMATTI, ANDREA, Bongiorno A., Mignoli M., Zamorani G., Lamareille F., Lanzuisi G., Miyaji T., Bolzonella M., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Lilly S. J., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Brusa M., Caputi K., Civano F., Coppa G., Cucciati O., de La Torre S., de Ravel L., Franzetti P., Garilli B., Halliday C., Hasinger G., Koekemoer A. M., Iovino A., Kampczyk P., Knobel C., Kova&#269, K., Le Borgne J.-F., Le Brun V., Maier C., Merloni A., Nair P., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Salvato M., Silverman J., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Guzzo L., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Scaramella R., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Astronomy
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), Surveys, 01 natural sciences, Luminosity, 0103 physical sciences, Galaxies: active, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Density evolution, 0105 earth and related environmental sciences, Line (formation), Luminosity function (astronomy), Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Redshift, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a catalog of 213 type-2 AGN selected from the zCOSMOS survey. The selected sample covers a wide redshift range (0.15, Comment: 20 pages, 11 figures, accepted for publication in Astronomy and Astrophysics
Published: 2010
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17. Tracking the impact of environment on the galaxy stellar mass function up to z â¼ 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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18. The Density Field of the 10k zCOSMOS Galaxies

Author: Kova, #269, Lilly S. J., Porciani C., Iovino A., Zamorani G., Oesch P., Bolzonella M., Knobel C., Finoguenov A., Peng Y., Carollo C. M., Pozzetti L., Caputi K., Silverman J. D., Tasca L. A. M., Scodeggio M., Vergani D., Scoville N. Z., Capak P., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Guzzo L., Kampczyk P., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pello R., Perez Montero E., Ricciardelli E., Tanaka M., Tresse L., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Fumana M., Koekemoer A. M., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Scaramella R., CUCCIATI, OLGA, CIMATTI, ANDREA, 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), Kova&#269, K., Lilly S. J., Cucciati O., Porciani C., Iovino A., Zamorani G., Oesch P., Bolzonella M., Knobel C., Finoguenov A., Peng Y., Carollo C. M., Pozzetti L.,Caputi K., Silverman J. D., Tasca L. A. M., Scodeggio M., Vergani D., Scoville N. Z., Capak P., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Guzzo L., Kampczyk P., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Perez Montero E., Ricciardelli E., Tanaka M., Tresse L., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Koekemoer A. M., Maccagni D., Marinoni C., McCracken H. J.,Memeo P., Meneux B., Scaramella R., Astronomy, and Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], LY-ALPHA EMITTERS, surveys, galaxies: high-redshift, 0103 physical sciences, LARGE-SCALE STRUCTURE, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, large-scale structure of universe, REDSHIFT SURVEY, 010308 nuclear & particles physics, Shot noise, Astronomy and Astrophysics, VLT DEEP SURVEY, ENVIRONMENTAL DEPENDENCE, Galaxy, Redshift, COSMOS FIELD, Space and Planetary Science, Galaxies: high-redshift, Large-scale structure of universe, Surveys, SMOOTHED PARTICLE HYDRODYNAMICS, LUMINOSITY DEPENDENCE, DIGITAL SKY SURVEY, STELLAR MASS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use the current sample of ~10,000 zCOSMOS spectra of sources selected with I(AB) < 22.5 to define the density field out to z~1, with much greater resolution in the radial dimension than has been possible with either photometric redshifts or weak lensing. We apply new algorithms that we have developed (ZADE) to incorporate objects not yet observed spectroscopically by modifying their photometric redshift probability distributions using the spectroscopic redshifts of nearby galaxies. This strategy allows us to probe a broader range of galaxy environments and reduce the Poisson noise in the density field. The reconstructed overdensity field of the 10k zCOSMOS galaxies consists of cluster-like patterns surrounded by void-like regions, extending up to z~1. Some of these structures are very large, spanning the ~50 Mpc/h transverse direction of the COSMOS field and extending up to Delta z~0.05 in redshift. We present the three dimensional overdensity maps and compare the reconstructed overdensity field to the independently identified virialised groups of galaxies and clusters detected in the visible and in X-rays. The distribution of the overdense structures is in general well traced by these virialised structures. A comparison of the large scale structures in the zCOSMOS data and in the mock catalogues reveals an excellent agreement between the fractions of the volume enclosed in structures of all sizes above a given overdensity between the data and the mocks in 0.2, Comment: 35 pages, 20 figures; submitted to ApJ; the high resolution pdf available at http://www.exp-astro.phys.ethz.ch/kovac/public/zCOSMOS
Published: 2010
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19. The zCOSMOS Redshift Survey: How group environment alters global downsizing trends

Author: Iovino A., Scodeggio M., Knobel C., Kova, #269, Lilly S., Bolzonella M., Tasca L. A. M., Zamorani G., Zucca E., Caputi K., Pozzetti L., Oesch P., Lamareille F., Halliday C., Bardelli S., Finoguenov A., Guzzo L., Kampczyk P., Maier C., Tanaka M., Vergani D., 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., Pellò R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Tresse L., Abbas U., Bottini D., Cappi A., Cassata P., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Schiminovich D., Scoville N., CUCCIATI, OLGA, CIMATTI, ANDREA, AUTRES, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), INAF- Milano, Istituto Nazionale di Astrofisica (INAF), Università di Bologna, Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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), INAF - Osservatorio Astronomico di Brera (OAB), INAF - Osservatorio Astronomico di Bologna (OABO), 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, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Tokai University, INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Chicago, Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (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), 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Space Telescope Science Institute (STSci), 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), California Institute of Technology (CALTECH), Iovino A., Cucciati O., Scodeggio M., Knobel C., Kova&#269, K., Lilly S., Bolzonella M., Tasca L. A. M., Zamorani G., Zucca E., Caputi K., Pozzetti L., Oesch P., Lamareille F., Halliday C., Bardelli S., Finoguenov A., Guzzo L., Kampczyk P., Maier C., Tanaka M., Vergani D., 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., Pellò R., Peng Y., Perez-Montero E., Ricciardelli E., Silverman J. D., Tresse L., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Schiminovich D., Scoville N., Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), 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 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), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Interactions, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Clusters, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxy formation and evolution, Mass segregation, Evolution - Galaxies, Galaxies, General - Galaxies, Astronomy and Astrophysics, Space and Planetary Science, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Redshift survey, Galaxy, Redshift, Low Mass, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We took advantage of the wealth of information provided by the first ~10000 galaxies of the zCOSMOS-bright survey and its group catalogue to study the complex interplay between group environment and galaxy properties. The classical indicator F_blue (fraction of blue galaxies) proved to be a simple but powerful diagnostic tool. We studied its variation for different luminosity and mass selected galaxy samples. Using rest-frame B-band selected samples, the groups galaxy population exhibits significant blueing as redshift increases, but maintains a lower F_blue with respect both to the global and the isolated galaxy population. However moving to mass selected samples it becomes apparent that such differences are largely due to the biased view imposed by the B-band luminosity selection, being driven by the population of lower mass, bright blue galaxies for which we miss the redder, equally low mass, counterparts. By focusing the analysis on narrow mass bins such that mass segregation becomes negligible we find that only for the lowest mass bin explored (logMass = 10.8 are already in place at z ~ 1 and do not exhibit any strong environmental dependence, possibly originating from so-called 'nature'/internal mechanisms. In contrast, for lower galaxy masses and redshifts lower than z ~ 1, we observe the emergence in groups of a population of 'nurture' red galaxies: slightly deviating from the trend of the downsizing scenario followed by the global galaxy population, and more so with cosmic time. These galaxies exhibit signatures of group-related secular physical mechanisms directly influencing galaxy evolution., Submitted to A&A, revised version after referee comments
Published: 2009
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20. An optical group catalogue to z = 1 from the zCOSMOS 10k sample

Author: Knobel, C., Lilly S. J., Iovino A., Porciani C., Kova, #269, Finoguenov A., Kitzbichler M. G., Carollo C. M., Contini T., Kneib J. P., LeFèvre O., Mainieri V., Renzini A., Scodeggio M., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Kampczyk P., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., 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., Fumana M., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Pozzetti L., Scaramella R., CUCCIATI, OLGA, CIMATTI, ANDREA, 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), 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), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), AUTRES, INAF- Milano, INAF - Osservatorio Astrofisico di Arcetri (OAA), 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), Knobel, C., Lilly S. J., Iovino A., Porciani C., Kova&#269, K., Cucciati O., Finoguenov A., Kitzbichler M. G., Carollo C. M., Contini T., Kneib J.-P., LeFèvre O., Mainieri V., Renzini A., Scodeggio M., Zamorani G., Bardelli S., Bolzonella M., Bongiorno A., Caputi K., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Kampczyk P., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., 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., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Pozzetti L., and Scaramella R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, galaxies: high-redshift, Galaxy group, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Group (mathematics), Velocity dispersion, Astronomy and Astrophysics, methods: data analysis, Redshift, Galaxy, Space and Planetary Science, galaxies: clusters: general, Catalogs, Galaxies: clusters: general, Galaxies: high-redshift, Methods: data analysis, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Instrumentation and Methods for Astrophysics, catalogs, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a galaxy group catalogue spanning the redshift range 0.1 = 5 spectroscopically confirmed members, with a further ~700 groups with 2, Comment: 20 pages, 19 figures, accepted for publication in ApJ
Published: 2009
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21. 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., Kneib J. P., Iovino A., Le Fèvre O., Kova, #269, Bolzonella M., Lilly S. J., Abraham R. G., Cassata P., Guzzo L., Tresse L., Zamorani G., Capak P., Garilli B., Scodeggio M., Sheth K., Zucca E., Carollo C. M., Contini T., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Caputi K., Coppa G., de La Torre S., de Ravel L., Franzetti P., Kampczyk P., Knobel C., Koekemoer A. M., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Vergani D., Tanaka M., Abbas U., Bottini D., Cappi A., Ilbert O., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Scaramella R., Scarlata C., CUCCIATI, OLGA, CIMATTI, ANDREA, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), AUTRES, INAF - Osservatorio Astronomico di Bologna (OABO), Mathématiques - Analyse, Probabilités, Modélisation - Orléans (MAPMO), Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), INAF- Milano, California Institute of Technology (CALTECH), Spitzer Science Center, California Institute of Technology, Pasadena, 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), Space Telescope Science Institute (STSci), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), 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), 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), 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), 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)-Université d'Orléans (UO), 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, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Tasca L. A. M., Kneib J.-P., Iovino A., Le Fèvre O., Kova&#269, K., Bolzonella M., Lilly S. J., Abraham R. G., Cassata P., Cucciati O., Guzzo L., Tresse L., Zamorani G., Capak P., Garilli B., Scodeggio M., Sheth K., Zucca E., Carollo C. M., Contini T., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Caputi K., Coppa G., de La Torre S., de Ravel L., Franzetti P., Kampczyk P., Knobel C., Koekemoer A. M., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Vergani D., Tanaka M., Abbas U., Bottini D., Cappi A., Cimatti A., Ilbert O., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Scaramella R., and Scarlata C.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Galaxy:formation, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Galaxies:structure, Galaxy group, 0103 physical sciences, Cosmology:large-scale structure of universe, Galaxies:distances and redshifts, Galaxies:evolution, Galaxies:fundamental parameters, Astronomy and Astrophysics, Space and Planetary Science, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Redshift survey, Galaxy, Universe, Redshift, 13. Climate action, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: For more than two decades we have known that galaxy morphological segregation is present in the Local Universe. It is important to see how this relation evolves with cosmic time. To investigate how galaxy assembly took place with cosmic time, we explore the evolution of the morphology-density relation up to redshift z~1 using about 10000 galaxies drawn from the zCOSMOS Galaxy Redshift Survey. Taking advantage of accurate HST/ACS morphologies from the COSMOS survey, of the well-characterised zCOSMOS 3D environment, and of a large sample of galaxies with spectroscopic redshift, we want to study here the evolution of the morphology-density relation up to z~1 and its dependence on galaxy luminosity and stellar mass. The multi-wavelength coverage of the field also allows a first study of the galaxy morphological segregation dependence on colour. We further attempt to disentangle between processes that occurred early in the history of the Universe or late in the life of galaxies. The zCOSMOS field benefits of high-resolution imaging in the F814W filter from the Advanced Camera for Survey (ACS). We use standard morphology classifiers, optimised for being robust against band-shifting and surface brightness dimming, and a new, objective, and automated method to convert morphological parameters into early, spiral, and irregular types. We use about 10000 galaxies down to I_AB=22.5 with a spectroscopic sampling rate of 33% to characterise the environment of galaxies up to z~1 from the 100 kpc scales of galaxy groups up to the 100 Mpc scales of the cosmic web. ABRIDGED, Comment: 23 pages, 12 figures, accepted for publication in Astronomy and Astrophysics
Published: 2009
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22. Evidence for major mergers of galaxies at 2 less than or similar to z \textless 4 in the VVDS and VUDS surveys

Author: Tasca, L. A. M., Le Fèvre, O., Lopez-Sanjuan, C., Wang, P. -W., Cassata, P., Garilli, B., Ilbert, O., Le Brun, V., Lemaux, B. C., Maccagni, D., Tresse, L., Bardelli, S., Contini, T., Charlot, S., Cucciati, O., Fontana, A., Giavalisco, M., Kneib, J. -P., Salvato, M., Taniguchi, Y., Vergani, D., Zamorani, G., Zucca, E., 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), AUTRES, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), INAF - Osservatorio Astronomico di Roma (OAR), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, INAF - Osservatorio Astrofisico di Arcetri (OAA), Oncology Institute of Southern Switzerland, European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), 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 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI)
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galaxies: high-redshift, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, Astrophysics::Galaxy Astrophysics
Abstract: International audience; Context. The mass assembly of galaxies can proceed through different physical processes. Here we report on the spectroscopic identification of close physical pairs of galaxies at redshifts 2 less than or similar to z \textless 4 and discuss the impact of major mergers in building galaxies at these early cosmological times. Aims. We aim to identify and characterize close physical pairs of galaxies destined to merge and use their properties to infer the contribution of merging processes to the early mass assembly of galaxies. Methods. We searched for galaxy pairs with a transverse separation r(p) \textless= 25 h(-1) kpc and a velocity difference Delta(v) \textless= 500 km s(-1) using early data from the VIMOS Ultra Deep Survey (VUDS) that comprise a sample of 1111 galaxies with spectroscopic redshifts measurements at redshifts 1.8 \textless= z \textless= 4 in the COSMOS. ECDFS, and VVDS-02h fields, combined with VVDS data. We analysed their spectra and associated visible and near-infrared photometry to assess the main properties of merging galaxies that have an average stellar mass M-* = 2.3 x 10(10) M-circle dot at these redshifts. Results. Using the 12 physical pairs found in our sample we obtain a first robust measurement of the major merger fraction at these redshifts, f(MM)= 19.4(-6)(+9)%. These pairs are expected to merge within 1 Gyr on average each producing a more massive galaxy by the time the cosmic star formation peaks at z similar to 1-2. Using the pairs' merging time scales, we derive a merging rate of R-MM = 0.17(-0.05)(+0.08) Gyr(-1). From the average mass ratio between galaxies in the pairs, the stellar mass of the resulting galaxy after merging will be similar to 60% higher than the most massive galaxy in the pair before merging. We conclude that major merging of galaxy pairs is on-going at 2 less than or similar to z \textless 4 and is significantly contributing to the major mass assembly phase of galaxies at this early epoch.
Published: 2014
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23. The zCOSMOS redshift survey: evolution of the light in bulges and discs since z similar to 0.8

Author: Tasca, L. A. M., Tresse, L., Le Fèvre, O., Ilbert, O., Lilly, S. J., Zamorani, G., Lopez-Sanjuan, C., Ho, L. C., Bardelli, S., Cattaneo, A., Cucciati, O., Farrah, D., Iovino, A., Koekemoer, A. M., Liu, C. T., Massey, R., Renzini, A., Taniguchi, Y., Welikala, N., Zucca, E., Carollo, C. M., Contini, T., Kneib, J. -P., Mainieri, V., Scodeggio, M., Bolzonella, M., Bongiorno, A., Caputi, K., Torre, S., Franzetti, P., Garilli, B., Guzzo, L., Kampczyk, P., Knobel, C., Kovac, K., Lamareille, F., Le Borgne, J. -F., Le Brun, V., Maier, C., Mignoli, M., Pello, R., Peng, Y., Perez Montero, E., Rich, Robert Michael, Tanaka, M., Vergani, D., Bordoloi, R., Cappi, A., Cimatti, Alessandro, Coppa, G., Mccracken, H. J., Moresco, M., Pozzetti, L., Sanders, D., Sheth, K., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Istituto Nazionale di Astrofisica (INAF), Kavli Institute for Astronomy and Astrophysics [Beijing] (KIAA-PKU), Peking University [Beijing], INAF - Osservatorio Astronomico di Bologna (OABO), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Department of Physics [Blacksburg], Virginia Tech [Blacksburg], INAF - Osservatorio Astronomico di Brera (OAB), Space Telescope Science Institute (STSci), City University of Hong Kong [Hong Kong] (CUHK), Institute for Computational Cosmology (ICC), Durham University, INAF - Osservatorio Astronomico di Padova (OAPD), Research Center for Space and Cosmic Evolution (RCSCE), Ehime University [Matsuyama, Japon], University of Chicago, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Ecole Polytechnique Fédérale de Lausanne (EPFL), European Southern Observatory (ESO), INAF- Milano, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Max-Planck-Institut für Extraterrestrische Physik (MPE), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], 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), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Department of Physics and Astronomy [UCLA Los Angeles], University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), National Astronomical Observatory of Japan (NAOJ), INAF - Osservatorio Astrofisico di Arcetri (OAA), 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), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), National Radio Astronomy Observatory (NRAO), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Università degli studi di Milano [Milano]-Università di Milano-Bicocca, Ehime University [Matsuyama], AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, University of California-University of California, Osservatorio Astronomico (INAF), 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), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), 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), 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: Galaxies: bulges, Galaxies: fundamental parameters, Galaxies: distances and redshifts, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galaxies: luminosity function, Mass function, Galaxies: evolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; We studied the chronology of galactic bulge and disc formation by analysing the relative contributions of these components to the B-band rest-frame luminosity density at different epochs. We present the first estimate of the evolution of the fraction of rest-frame B-band light in galactic bulges and discs since redshift z similar to 0.8. We performed a bulge-to-disc decomposition of HST/ACS images of 3266 galaxies in the zCOSMOS-bright survey with spectroscopic redshifts in the range 0.7 \textless= z \textless= 0.9. We find that the fraction of B-band light in bulges and discs is (26 4)% and (74 4)%, respectively. When compared with rest-frame B-band measurements of galaxies in the local Universe in the same mass range (10(9)M circle dot M10(11.5).M circle dot),we find that the B-band light in discs decreases by -30% from z similar to 0.7-0.9 to z 0, while the light from the bulge increases by -30% over the same period of time. We interpret this evolution as the consequence of star formation and mass assembly processes, as well as morphological transformation, which gradually shift stars formed at half the age of the Universe from star-forming late-type/irregular galaxies to earlier types and ultimately into spheroids.
Published: 2014
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24. VVDS-SWIRE. Clustering evolution from a spectroscopic sample of galaxies with redshift 0.2 < z < 2.1 selected from Spitzer IRAC 3.6 μ m and 4.5 μ m photometry

Author: de La Torre S., Le Fèvre O., Arnouts S., Guzzo L., Farrah D., Iovino A., Lonsdale C. J., Meneux B., Oliver S. J., Pollo A., Waddington I., Bottini D., Fang F., Garilli B., Le Brun V., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Shupe D., Surace J., Tresse L., Vettolani G., Zanichelli A., Adami C., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Lamareille F., McCracken H. J., Marinoni C., Mazure A., Merighi R., Paltani S., Pellò R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Brinchmann J., Mellier Y., Merluzzi P., Temporin S., Vergani D., Walcher C. J., MARANO, BRUNO, BONGIORNO, ANGELA, CUCCIATI, OLGA, de La Torre S., Le Fèvre O., Arnouts S., Guzzo L., Farrah D., Iovino A., Lonsdale C. J., Meneux B., Oliver S. J., Pollo A., Waddington I., Bottini D., Fang F., Garilli B., Le Brun V., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Shupe D., Surace J., Tresse L., Vettolani G., Zanichelli A., Adami C., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Lamareille F., McCracken H. J., Marano B., Marinoni C., Mazure A., Merighi R., Paltani S., Pellò R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Brinchmann J., Cucciati O., Mellier Y., Merluzzi P., Temporin S., Vergani D., and Walcher C. J.
Subjects: Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Aims.By combining data from the VIMOS VLT Deep Survey (VVDS) with the Spitzer Wide-area InfraRed Extragalactic survey (SWIRE) we have built the currently largest spectroscopic sample of high redshift galaxies selected in the rest-frame near-infrared. We have obtained 2040 spectroscopic redshifts of galaxies with (m3.6)_AB < 21.5 at 3.6 μ m and 1255 spectroscopic redshifts of galaxies with (m4.5)_AB < 21. These allow us to investigate the clustering evolution of galaxies selected via their rest-frame near-infrared luminosity in the redshift range 0.2 < z < 2.1. Methods: We use the projected two-point correlation function w_p(r_p) to study the three dimensional clustering properties of galaxies detected at 3.6 μ m and 4.5 μ m with the InfraRed Array Camera (IRAC) in the SWIRE survey with measured spectroscopic redshifts from the first epoch VVDS. We compare these properties to those of a larger sample of 16672 SWIRE galaxies for which we have accurate photometric redshifts in the same field. Results: We find that in the 3.6 μ m and 4.5 μ m flux limited samples the apparent correlation length does not change from redshift ~2 to the present. The measured correlation lengths have a mean value of r0 ≃ 3.9±0.5 h-1 Mpc for the galaxies selected at 3.6 μ m and a mean value of r0 ≃ 4.4±0.5 h-1 Mpc for the galaxies selected at 4.5 μ m across the whole redshift range explored. These values are larger than those typicaly found for I-band selected galaxies at I_AB < 24 for which r0 varies from 2.69 h-1 Mpc to 3.63 h-1 Mpc between z = 0.5 to z = 2.1. We find that the difference in correlation length between I-band and 3.6-4.5 μm selected samples decreases with increasing redshift becoming comparable at z ≃ 1.5. We interpret this as evidence that galaxies with older stellar populations and galaxies actively forming stars reside in comparably over-dense environments at epochs earlier than z ≃ 1.5 supporting the recently reported flattening of the color-density relation at high redshift. The increasing difference in correlation length with cosmic time observed between rest-frame UV-optical and near-infrared selected samples could then be an indication that star formation is gradually shifting to lower density regions with decreasing redshift while the older passively evolving galaxies remain in the most over-dense peaks.
Published: 2007

25. The VIMOS-VLT Deep Survey: the build-up of the colour density relation

Author: CUCCIATI, OLGA, MARANO, BRUNO, BONGIORNO, ANGELA, GREGORINI, LORETTA, Iovino A., Marinoni C., Ilbert O., Bardelli S., Franzetti P., Le Fèvre O., Pollo A., Zamorani G., Cappi A., Guzzo L., McCracken H. J., Meneux B., Scaramella R., Scodeggio M., Tresse L., Zucca E., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J. P., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Gavignaud I., Mazure A., Merighi R., Paltani S., Pellò R., Pozzetti L., Radovich M., Bondi M., Busarello G., de La Torre S., Lamareille F., Mathez G., Mellier Y., Merluzzi P., Ripepi V., Rizzo D., Temporin S., Vergani D., Cucciati O., Iovino A., Marinoni C., Ilbert O., Bardelli S., Franzetti P., Le Fèvre O., Pollo A., Zamorani G., Cappi A., Guzzo L., McCracken H. J., Meneux B., Scaramella R., Scodeggio M., Tresse L., Zucca E., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J. P., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Gavignaud I., Marano B., Mazure A., Merighi R., Paltani S., Pellò R., Pozzetti L., Radovich M., Bondi M., Bongiorno A., Busarello G., de La Torre S., Gregorini L., Lamareille F., Mathez G., Mellier Y., Merluzzi P., Ripepi V., Rizzo D., Temporin S., and Vergani D.
Subjects: GALAXIES: EVOLUTION, LARGE SCALE STRUCTURE OF UNIVERSE, COSMOLOGY: OBSERVATIONS, GALAXIES: STATISTICS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, GALAXIES: DISTANCES AND REDSHIFTS
Abstract: We investigate the redshift and luminosity evolution of the galaxy colour-density relation using the data from the First Epoch VIMOS-VLT Deep Survey (VVDS). The size (6582 galaxies with good quality redshifts), depth (IAB&leq; 24) and redshift sampling rate (20% on the mean) of the survey enable us to reconstruct the 3D galaxy environment on relatively local scales (R=5 h-1 Mpc) up to redshift z ˜ 1.5. Particular attention has been devoted to calibrate a density reconstruction scheme, which factors out survey selection effects and reproduces in an unbiased way the underlying "real" galaxy environment. We find that the colour-density relation shows a dramatic change as a function of cosmic time. While at lower redshift we confirm the existence of a steep colour-density relation, with the fraction of the reddest(/bluest) galaxies of the same luminosity increasing(/decreasing) as a function of density, this trend progressively disappears in the highest redshift bins investigated. Our results suggest the existence of an epoch (more remote for brighter galaxies) characterized by the absence of the colour-density relation on the R=5 h-1 Mpc scales investigated. The rest frame u*-g' colour-magnitude diagram shows a bimodal pattern in both low and high density environments up to redshift z˜ 1.5. We find that the bimodal distribution is not universal but strongly depends upon environment: at lower redshifts the colour-magnitude diagrams in low and high density regions are significantly different while the progressive weakening of the colour-density relation causes the two bimodal distributions to nearly mirror each other in the highest redshift bin investigated. Both the colour-density and the colour-magnitude-density relations, on the R=5 h-1 Mpc scales, appear to be a transient, cumulative product of genetic and environmental factors that have been operating over at least a period of 9 Gyr. These findings support an evolutionary scenario in which star formation/gas depletion processes are accelerated in more luminous objects and in high density environments: star formation activity is progressively shifting with cosmic time towards lower luminosity galaxies (downsizing), and out of high density environments.
Published: 2006

26. The VIMOS VLT Deep Survey: A new window on the distant universe

Author: Le Fèvre, O., Vettolani, G., Bianca Garilli, Tresse, L., Bottini, D., Le Brun, V., Maccagni, D., Picat, J. -P, Scaramella, R., Scodeggio, M., Zanichelli, A., Adami, C., Arnaboldi, M., Arnouts, S., Bardelli, S., Bolzonella, M., Cappi, A., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Gavignaud, I., Guzzo, L., Ilbert, O., Iovino, A., Mccracken, H. J., Marano, B., Marinoni, C., Mathez, G., Mazure, A., Meneux, B., Merighi, R., Paltani, S., Pelló, R., Pollo, A., Pozzetti, L., Radovich, M., Zamorani, G., Zucca, E., Bondi, M., Bongiorno, A., Busarello, G., Mellier, Y., Merluzzi, P., Ripepi, V., Rizzo, D., 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), F. Casoli, T. Contini, J.M. Hameury and L. Pagani, 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), Università di Bologna, Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), J.M. Hameury and L. Pagani., EDITED BY F. CASOLI, T. CONTINI, J.M. HAMEURY AND L. PAGANI., Le Fèvre O., Vettolani G., Garilli B., Tresse L., Bottini D., Le Brun V., Maccagni D., Picat J.-P., Scaramella R., Scodeggio M., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Ilbert O., Iovino A., McCracken H. J., Marano B., Marinoni C., Mathez G., Mazure A., Meneux B., Merighi R., Paltani S., Pelló R., Pollo A., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: To appear in The Fabulous Destiny of Galaxies: Bridging Past and Present, conference held in Marseille, June 2005; The First Epoch VIMOS VLT Deep Survey is now completed. More than 11000 redshifts of galaxies with 17.5 &leq; IAB &leq; 24 have been measured with the VIMOS spectrograph build for ESO by our consortium of French and Italian Institutes. The magnitude selection of this survey is unique and allows an unprecedented census of the high redshift universe to trace the evolution of galaxies and AGNs from 12 billion years ago to the present. We present here the main results from this first epoch survey. A first public data release offers access to the deep imaging and to 1599 galaxies with redshifts in the Chandra Deep Field South. The VVDS continues beyond the first epoch, a total of more than 45000 spectra have been obtained and processing is on-going.
Published: 2005

27. The VIMOS VLT Deep Survey - The evolution of galaxy clustering to z=2 from first epoch observations

Author: Le Fèvre O., Guzzo L., Meneux B., Pollo A., Cappi A., Colombi S., Iovino A., Marinoni C., McCracken H. J., Scaramella R., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J. P., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Blaizot J., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Mathez G., Mazure A., Merighi R., Paltani S., Pellò R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Busarello G., Lamareille F., Mellier Y., Merluzzi P., Ripepi V., Rizzo D. ns Astronomy, Astrophysics Volume 439 Issue 3 September I. 2005 p.p. 877 885, MARANO, BRUNO, BONGIORNO, ANGELA, 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), 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), Le Fèvre O., Guzzo L., Meneux B., Pollo A., Cappi A., Colombi S., Iovino A., Marinoni C., McCracken H. J., Scaramella R., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J. P., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Blaizot J., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Marano B., Mathez G., Mazure A., Merighi R., Paltani S., Pellò R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Lamareille F., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D. ns Astronomy and Astrophysics Volume 439 Issue 3 September I 2005 pp.877-885
Subjects: GALAXIES: EVOLUTION, molecular data, Dark matter, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, infrared: ISM, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), COSMOLOGY:: LARGE SCALE STRUCTURE OF UNIVERSE, Astronomy and Astrophysics, Billion years, Galaxy, Redshift, ISM: molecules, Correlation function (statistical mechanics), Space and Planetary Science, ISM: individual objects: W49, Magnitude (astronomy), SURVEYS, ISM: individual objects: Sagittarius B2
Abstract: This paper presents the evolution of the clustering of the main population of galaxies from z=2.1 to z=0.2, from the first epoch VIMOS VLT Deep Survey (VVDS), a magnitude limited sample with 17.5, 11 pages, accepted 11-Apr-05 in A&A
Published: 2005
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28. THE COLORS OF CENTRAL AND SA℡LITE GALAXIES IN zCOSMOS OUT TO z similar or equal to 0.8 AND IMPLICATIONS FOR QUENCHING

Author: Knobel, C., Lilly, S. J., Kovac, K., Peng, Y., Bschorr, T. J., Carollo, C. M., Contini, T., Kneib, J. -P., Le Fevre, O., Mainieri, V., Renzini, A., Scodeggio, M., Zamorani, G., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Cucciati, O., Torre, S., Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Lamareille, F., Le Borgne, J. -F., Le Brun, V., Maier, C., Mignoli, M., Pello, R., Perez Montero, E., Presotto, V., Silverman, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., BARNES, L., Bordoloi, R., Cappi, A., Cimatti, Alessandro, Coppa, G., Koekemoer, A. M., Lopez-Sanjuan, C., McCracken, H. J., Moresco, M., Nair, P., Pozzetti, L., Welikala, N., 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), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; We examine the red fraction of central and satellite galaxies in the large zCOSMOS group catalog out to z similar or equal to 0.8, correcting for both the incompleteness in stellar mass and for the less than perfect purities of the central and satellite samples. We show that at all masses and at all redshifts, the fraction of satellite galaxies that have been quenched, i.e., that are red, is systematically higher than that of centrals, as seen locally in the Sloan Digital Sky Survey (SDSS). The satellite quenching efficiency, which is the probability that a satellite is quenched because it is a satellite rather than a central, is, as locally, independent of stellar mass. Furthermore, the average value is about 0.5, which is also very similar to that seen in the SDSS. We also construct the mass functions of blue and red centrals and satellites and show that these broadly follow the predictions of the Peng et al. analysis of the SDSS groups. Together, these results indicate that the effect of the group environment in quenching satellite galaxies was very similar to what it is today when the universe was about half its present age.
Published: 2013
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29. The VIMOS VLT Deep Survey: the redshift distribution N(z) of magnitude-limited samples down to iAB=24.75 and KsAB=22

Author: Le Fevre, O., Cassata, P., Cucciati, O., La Torre, S., Garilli, B., Ilbert, O., Le Brun, V., Maccagni, D., Tresse, L., Zamorani, G., Bardelli, S., Bolzonella, M., Contini, T., Iovino, A., Lopez-Sanjuan, C., Mccracken, H. J., Pollo, A., Pozzetti, L., Scodeggio, M., Tasca, L., Vergani, D., Alessandra Zanichelli, and Zucca, E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure and analyse the redshift distribution N(z) of magnitude-selected samples using spectroscopic redshift measurement from the magnitude-selected VIMOS VLT Deep Survey (VVDS) with 172. Down to iAB2 than in colour-colour selected samples, and we use the magnitude-selected VVDS to emphasize the large uncertainties associated to other surveys using colour or colour-colour selected samples. Our results further demonstrate that semi-analytical models on dark matter simulations have yet to find the right balance of physical processes and time-scales to properly reproduce a fundamental galaxy population property like the observed N(z)., Comment: Submitted to Astronomy and Astrophysics
Published: 2013
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30. The zCOSMOS-Bright survey: the clustering of early and late galaxy morphological types since z similar or equal to 1

Author: de la Torre, S., Le Fevre, O., Porciani, C., Guzzo, L., Meneux, B., Abbas, U., Tasca, L., Carollo, C. M., Contini, T., Kneib, J. -P., Lilly, S. J., Mainieri, V., Renzini, A., Scodeggio, M., Zamorani, G., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Coppa, G., Cucciati, O., de Ravel, L., Franzetti, P., Garilli, B., Halliday, C., Iovino, A., Kampczyk, P., Knobel, C., Koekemoer, A. M., Kovac, K., Lamareille, F., Le Borgne, J. -F., Le Brun, V., Maier, C., Mignoli, M., Pello, R., Peng, Y., Perez-Montero, E., Ricciardelli, E., Silverman, J., Tanaka, M., Tresse, L., Vergani, D., Zucca, E., Bottini, D., Cappi, A., Cassata, P., Cimatti, A., Leauthaud, A., Maccagni, D., Marinoni, C., McCracken, H. J., Memeo, P., Oesch, P., Pozzetti, L., Scaramella, R., and Astronomy
Subjects: REDSHIFT SURVEY, DIGITAL-SKY-SURVEY, 2-POINT CORRELATION-FUNCTION, Astrophysics::Cosmology and Extragalactic Astrophysics, VLT DEEP SURVEY, ENVIRONMENTAL DEPENDENCE, COLD DARK-MATTER, SPECTRAL TYPE, galaxies: high-redshift, cosmology: observations, LARGE-SCALE STRUCTURE, SPECTROSCOPIC SAMPLE, LUMINOSITY DEPENDENCE, large-scale structure of Universe, galaxies: evolution, Astrophysics::Galaxy Astrophysics, galaxies: statistics
Abstract: We measure the spatial clustering of galaxies as a function of their morphological type at z similar or equal to 0.8, for the first time in a deep redshift survey with full morphological information. This is obtained by combining high-resolution Hubble Space Telescope imaging and Very Large Telescope spectroscopy for about 8500 galaxies to with accurate spectroscopic redshifts from the zCOSMOS-Bright redshift survey. At this epoch, early-type galaxies already show a significantly stronger clustering than late-type galaxies on all probed scales. A comparison to the Sloan Digital Sky Survey Data at z similar or equal to 0.1 shows that the relative clustering strength between early and late morphological classes tends to increase with cosmic time at small separations, while on large scales it shows no significant evolution since z similar or equal to 0.8. This suggests that most early-type galaxies had already formed in intermediate and dense environments at this epoch. Our results are consistent with a picture in which the relative clustering of different morphological types between z similar or equal to 1 and 0 reflects the evolving role of environment in the morphological transformation of galaxies, on top of a global evolution driven by mass.
Published: 2011

31. The zCOSMOS-Bright survey: the clustering of early and late galaxy morphological types since z≃ 1

Author: De La Torre, S., Le Fèvre, O., Porciani, C., Guzzo, L., Meneux, B., Abbas, U., Tasca, L., Carollo, C. M., Contini, T., Kneib, J.-P., Lilly, S. J., Mainieri, V., Renzini, A., Scodeggio, M., Zamorani, G., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Coppa, G., Cucciati, O., De Ravel, L., Franzetti, P., Garilli, B., Halliday, C., Iovino, A., Kampczyk, P., Knobel, C., Koekemoer, A. M., Kovač, K., Lamareille, F., Le Borgne, J.-F., Le Brun, V., Maier, C., Mignoli, M., Pelló, R., Peng, Y., Perez-Montero, E., Ricciardelli, E., Silverman, J., Tanaka, M., Tresse, L., Vergani, D., Zucca, E., Bottini, D., Cappi, A., Cassata, P., Cimatti, Alessandro, Leauthaud, A., Maccagni, D., Marinoni, Christian, McCracken, H. J., Memeo, P., Oesch, P., Pozzetti, L., Scaramella, R., 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 Torino (OATo), Istituto Nazionale di Astrofisica (INAF), 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), Ecole Polytechnique Fédérale de Lausanne (EPFL), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), European Southern Observatory (ESO), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], AUTRES, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Institut de recherche en astrophysique et planétologie (IRAP), Laboratoire Léon Brillouin (LLB - UMR 12), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Hunan Normal University (HNU), INAF - Osservatorio Astrofisico di Arcetri (OAA), Joseph Louis LAGRANGE (LAGRANGE), 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), California Institute of Technology (CALTECH), 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), 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), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Hunan Normal University, 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), 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: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure the spatial clustering of galaxies as a function of their morphological type at z~0.8, for the first time in a deep redshift survey with full morphological information. This is obtained by combining high-resolution HST imaging and VLT spectroscopy for about 8,500 galaxies to I_AB=22.5 with accurate spectroscopic redshifts from the zCOSMOS-Bright redshift survey. At this epoch, early-type galaxies already show a significantly stronger clustering than late-type galaxies on all probed scales. A comparison to the SDSS at z~0.1, shows that the relative clustering strength between early and late morphological classes tends to increase with cosmic time at small separations, while on large scales it shows no significant evolution since z~0.8. This suggests that most early-type galaxies had already formed in intermediate and dense environments at this epoch. Our results are consistent with a picture in which the relative clustering of different morphological types between z~1 and z~0, reflects the evolving role of environment in the morphological transformation of galaxies, on top of the global mass-driven evolution., Comment: 10 pages, 10 figures, accepted for publication in MNRAS
Published: 2011
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32. The power spectrum from the angular distribution of galaxies in the CFHTLS-Wide fields at redshift ~0.7

Author: Krywult, J., Le Brun, V., Le Fevre, O., Maccagni, D., Malek, K., Marulli, F., Meneux, B., Paioro, L., Polletta, M., Pollo, A., Scodeggio, M., Schlagenhaufer, H., Tasca, L., Tojeiro, R., Vergani, D., Zanichelli, A., Granett, B.~R., Guzzo, L., Coupon, J., Arnouts, S., Hudelot, P., Ilbert, O., McCracken, H.~J., Mellier, Y., Adami, C., Bel, Julien, Bolzonella, M., Bottini, D., Cappi, A., Cucciati, O., Torre, S., Franzetti, P., Fritz, A., Garilli, B., Iovino, A., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), B. R. Granett, L. Guzzo, J. Coupon, S. Arnout, P. Hudelot, O. Ilbert, H. J. McCracken, Y. Mellier, C. Adami, J. Bel, M. Bolzonella, D. Bottini, A. Cappi, O. Cucciati, S. de la Torre, P. Franzetti, A. Fritz, B. Garilli, A. Iovino, J. Krywult, V. Le Brun, O. Le Fevre, D. Maccagni, K. Malek, F. Marulli, B. Meneux, L. Paioro, M. Polletta, A. Pollo, M. Scodeggio, H. Schlagenhaufer, L. Tasca, R. Tojeiro, D. Vergani, A. Zanichelli, and University of St Andrews. School of Physics and Astronomy
Subjects: Cosmology and Gravitation, statistical [Methods], methods: statistical, cosmology: observation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, QC Physics, cosmology: observations, QB Astronomy, [INFO]Computer Science [cs], large-scale structure of Universe, observations [Cosmology], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], QC, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, QB, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure the real-space galaxy power spectrum on large scales at redshifts 0.5 to 1.2 using optical colour-selected samples from the CFHT Legacy Survey. With the redshift distributions measured with a preliminary ~14000 spectroscopic redshifts from the VIMOS Public Extragalactic Redshift Survey (VIPERS), we deproject the angular distribution and directly estimate the three-dimensional power spectrum. We use a maximum likelihood estimator that is optimal for a Gaussian random field giving well-defined window functions and error estimates. This measurement presents an initial look at the large-scale structure field probed by the VIPERS survey. We measure the galaxy bias of the VIPERS-like sample to be b_g=1.38 +- 0.05 (sigma_8=0.8) on scales k, Comment: Minor changes to match journal version
Published: 2011
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33. Understanding the shape of the galaxy two-point correlation function at z ~= 1 in the COSMOS field

Author: de la Torre, S., Guzzo, L., Kovač, K., Porciani, C., Abbas, U., Meneux, B., Carollo, C. M., Contini, T., Kneib, J. P., Le Fèvre, O., Lilly, S. J., Mainieri, V., Renzini, A., Sanders, D., Scodeggio, M., Scoville, N., Zamorani, G., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Coppa, G., Cucciati, O., de Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Koekemoer, A. M., Lamareille, F., Le Borgne, J.-F, Le Brun, V., Maier, C., Mignoli, M., Pelló, R., Peng, Y., Perez-Montero, E., Ricciardelli, E., Silverman, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Welikala, N., Zucca, E., Bottini, D., Cappi, A., Cassata, P., Cimatti, A., Fumana, M., Ilbert, O., Leauthaud, A., Maccagni, D., Marinoni, C., McCracken, H. J., Memeo, P., Nair, P., Oesch, P., Pozzetti, L., Presotto, V., Scaramella, R., 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: galaxies: high-redshift, cosmology: observations, [INFO]Computer Science [cs], Astrophysics::Cosmology and Extragalactic Astrophysics, large-scale structure of Universe, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, evolution, galaxies: statistics, large-scale structure of Universe [galaxies], ComputingMilieux_MISCELLANEOUS
Abstract: Monthly Notices of the Royal Astronomical Society, 409 (2), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711
Published: 2010
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34. The VIMOS-VLT Deep Survey: History of the Galaxy Clustering in the Universe

Author: Pollo, Agnieszka, Abbas, U., Meneux, B., Guzzo, L., Le Fèvre, O., De La Torre, S., Cappi, A., Garilli, B., Marinoni, C., Bottini, D., Le Brun, V., Maccagni, D., Scodeggio, M., Tresse, L., Vettolani, G., Zanichelli, A., Adami, C., Arnouts, S., Bardelli, S., Bolzonella, M., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Gavignaud, I., Ilbert, O., Iovino, A., McCracken, H.J., Mazure, A., Merighi, R., Paltani, S., Pellò, R., Pozzetti, L., Vergani, D., Zamorani, G., and Zucca, E.
Subjects: Physics, Galaxy group, Elliptical galaxy, Galaxy formation and evolution, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy merger, Interacting galaxy, Brightest cluster galaxy, Lenticular galaxy, Astrophysics::Galaxy Astrophysics, Dwarf galaxy
Abstract: Star formation in galaxies and their evolution depends on their local environment and, more precisely, their location in the large scale structure. The data from the VIMOS‐VLT Deep Survey (VVDS) has enabled us to investigate the history of the galaxy clustering and the relation between the evolution of galaxies themselves and the galaxy clustering back to z∼1. We analyzed the evolution of the projected two‐point correlation function for particular galaxy classes, with different intrinsic luminosities and stellar masses. We concluded that the properties of central and satellite galaxies in the dark matter haloes could have changed significantly between z∼1 and now.
Published: 2010
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35. Testing gravity on large scales. The skewness of the galaxy distribution at z~1

Author: Marinoni, C., Guzzo, L., Cappi, A., Le Fevre, O., Mazure, A., Meneux, B., Pollo, A., Iovino, A., Mccracken, H. J., Roberto Scaramella, La Torre, S., Virey, J. M., Bottini, D., Garilli, B., Le Brun, V., Maccagni, D., Picat, J. P., Scodeggio, M., Tresse, L., Vettolani, G., Zanichelli, A., Adami, C., Arnouts, S., Bardelli, S., Bolzonella, M., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Gavignaud, I., Ilbert, O., Lamareille, F., Marano, B., Mathez, G., Merighi, R., Paltani, S., Pellò, R., Pozzetti, L., Radovich, M., Vergani, D., Zamorani, G., Zucca, E., Abbas, U., Bondi, M., Bongiorno, A., Brinchmann, J., Buzzi, A., Cucciati, O., Ravel, L., Gregorini, L., Mellier, Y., Merluzzi, P., Perez-Montero, E., Taxil, P., Temporin, S., Walcher, C. J., 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), AUTRES, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Capodimonte (OAC), 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), INAF - Osservatorio Astronomico di Bologna (OABO), 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), INAF- Milano, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (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), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Services communs OMP - UMS 831 (UMS 831), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Toulouse III - Paul Sabatier (UT3), Università di Bologna, Dipartimento di Astronomia, Università di Bologna [Bologna] (UNIBO), Centre d'Economie et de Sociologie Rurales Appliquées à l'Agriculture et aux Espaces Ruraux (CESAER), Institut National de la Recherche Agronomique (INRA)-AgroSup Dijon - Institut National Supérieur des Sciences Agronomiques, de l'Alimentation et de l'Environnement, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Brera (INAF), European Southern Observatory (ESO), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, INAF - Osservatorio Astronomico di Bologna (OAB), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto di Radioastronomia (IRA), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto [Porto], Dipartimento di Fisica, Università degli studi di Milano [Milano]-Università di Milano-Bicocca, Departement de Radioastronomie Millimétrique (DEMIRM), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Biology, University of Washington [Seattle], 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 National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), 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), Services communs OMP (UMS 831), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Etablissement National d'Enseignement Supérieur Agronomique de Dijon (ENESAD)-Institut National de la Recherche Agronomique (INRA), INAF - Osservatorio Astronomico di Brera (OAB), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Istituto di Radioastronomia [Bologna] (IRA), Universidade do Porto, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Bernardo, Elizabeth, 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 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), Universidade do Porto = University of Porto, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), and École normale supérieure - Paris (ENS-PSL)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: We study the evolution of the low-order moments of the galaxy overdensity distribution over the redshift interval 0.7, Comment: To appear in the proceedings of 43rd Rencontres de Moriond on Cosmology (La Thuile, 2008)
Published: 2008

36. The VIRMOS-VLT Deep Survey: the last 10 billion years of evolution of galaxy clustering

Author: Pollo, A., Guzzo, L., Le Fèvre, O., Meneux, B., Cappi, A., Mccracken, H. J., Iovino, A., Marinoni, C., Bottini, D., Garilli, B., Le Brun, V. L., Maccagni, D., Picat, J. P., Scaramella, R., Marco Scodeggio, Tresse, L., Vettolani, G., Zanichelli, A., Adami, C., Arnouts, S., Bardelli, S., Bolzonella, M., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Gavignaud, I., Ilbert, O., Marano, B., Mazure, A., Merighi, R., Paltani, S., Pellò, R., Pozzetti, L., Radovich, M., Zamorani, G., Zucca, E., Bondi, M., Bongiorno, A., Brinchmann, J., Cucciati, O., La Torre, S., Lamareille, F., Mellier, Y., Merluzzi, P., Temporin, S., Vergani, D., Walcher, C. J., INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), 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), A. Pollo, L. Guzzo, O. Le Fevre, B. Meneux, A. Cappi, H. J. McCracken, A. Iovino, C. Marinoni, D. Bottini, B. Garilli, V. L. Le, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnout, S. Bardelli, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, O. Ilbert, B. Marano, A. Mazure, R. Merighi, S. Paltani, R. Pello, L. Pozzetti, M. Radovich, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, O. Cucciati, S. . la, F. Lamareille, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, C. J. Walcher, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], SPECTRAL TYPE, VIMOS, LUMINOSITY, DEPENDENCE, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We discuss the evolution of clustering of galaxies in the Universe from the present epoch back to z ~ 2, using the first-epoch data from the VIMOS-VLT Deep Survey (VVDS). We present the evolution of the projected two-point correlation function of galaxies for the global galaxy population, as well as its dependence on galaxy intrinsic luminosities and spectral types. While we do not find strong variations of the correlation function parameters with redshift for the global galaxy population, the clustering of objects with different intrinsic luminosities evolved significantly during last 8-10 billion years. Our findings indicate that bright galaxies in the past traced higher density peaks than they do now and that the shape of the correlation function of most luminous galaxies is different from observed for their local counterparts, which is a supporting evidence of a non-trivial evolution of the galaxy vs. dark matter bias., Comment: 4 pages, 4 figures, to appear in the proceedings of the conference 'At the Edge of the Universe' (9-13 October 2006, Sintra, Portugal)
Published: 2006

37. First results from the VIMOS/VLT Deep Survey (VVDS): luminosity functions from z̃0 to z̃1.5

Author: Zucca, E., Ilbert, O., Tresse, L., Bardelli, S., Arnouts, S., Zamorani, G., Le Fèvre, O., Vettolani, G., Adami, C., Sbolzonella, M., Bondi, M., Bongiorno, A., Bottini, D., Busarello, G., Cappi, A., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Garilli, B., Gavignaud, I., Gregorini, L., Guzzo, L., Iovino, A., Le Brun, V., Maccagni, D., Marano, B., Marinoni, C., Mathez, G., Mazure, A., Mccracken, H. J., Mellier, Y., Meneux, B., Merighi, R., Merluzzi, P., Paltani, S., Pellò, R., Picat, J. P., Pollo, A., Pozzetti, L., Radovich, M., Ripepi, V., Rizzo, D., Scaramella, R., Marco Scodeggio, Zanichelli, A., Zucca E., Ilbert O., Tresse L., Bardelli S., Arnouts S., Zamorani G., Le Fèvre O., Vettolani G., Adami C., Bolzonella M., Bondi M., Bongiorno A., Bottini D., Busarello G., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Garilli B., Gavignaud I., Gregorini L., Guzzo L., Iovino A., Le Brun V., Maccagni D., Marano B., Marinoni C., Mathez G., Mazure A., McCracken H. J., Mellier Y., Meneux B., Merighi R., Merluzzi P., Paltani S., Pellò R., Picat J. P., Pollo A., Pozzetti L., Radovich M., Ripepi V., Rizzo D., Scaramella R., Scodeggio M., and Zanichelli A.
Subjects: GALAXIES: REDSHIFTS, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The VIMOS/VLT Deep Survey (VVDS) is an on-going program to map the evolution of galaxies, large scale structures and AGNs from the redshift measurement of more than 100000 objects down to a magnitude IAB=24, in combination with a multi-wavelength dataset from radio to X-rays. We present here the results obtained from the first epoch data, regarding in particular the evolution of the luminosity function.

38. The BigBOSS Experiment

Author: Schlegel, D., Abdalla, F., Abraham, T., Ahn, C., Allende Prieto, C., Annis, J., Aubourg, E., Azzaro, M., Baltay, S. Bailey C., Baugh, C., Bebek, C., Becerril, S., Blanton, M., Bolton, A., Bromley, B., Cahn, R., Carton, P. -H, Cervantes-Cota, J. L., Chu, Y., Cortes, M., Dawson, K., Dey, A., Dickinson, M., Diehl, H. T., Doel, P., Ealet, A., Edelstein, J., Eppelle, D., Escoffier, S., Evrard, A., Faccioli, L., Frenk, C., Geha, M., Gerdes, D., Gondolo, P., Gonzalez-Arroyo, A., Grossan, B., Heckman, T., Heetderks, H., Ho, S., Honscheid, K., Huterer, D., Ilbert, O., Ivans, I., Jelinsky, P., Jing, Y., Joyce, D., Kennedy, R., Kent, S., Kieda, D., Kim, A., Kim, C., Kneib, J. -P, Kong, X., Kosowsky, A., Krishnan, K., Lahav, O., Lampton, M., Lebohec, S., Le Brun, V., Levi, M., Li, C., Liang, M., Lim, H., Lin, W., Linder, E., Lorenzon, W., La Macorra, A., Magneville, Ch, Malina, R., Marinoni, C., Martinez, V., Majewski, S., Matheson, T., Mccloskey, R., Mcdonald, P., Mckay, T., Mcmahon, J., Menard, B., Miralda-Escude, J., Modjaz, M., Montero-Dorta, A., Morales, I., Mostek, N., Newman, J., Nichol, R., Peter Nugent, Olsen, K., Padmanabhan, N., Palanque-Delabrouille, N., Park, I., Peacock, J., Percival, W., Perlmutter, S., Peroux, C., Petitjean, P., Prada, F., Prieto, E., Prochaska, J., Reil, K., Rockosi, C., Roe, N., Rollinde, E., Roodman, A., Ross, N., Rudnick, G., Ruhlmann-Kleider, V., Sanchez, J., Sawyer, D., Schimd, C., Schubnell, M., Scoccimaro, R., Seljak, U., Seo, H., Sheldon, E., Sholl, M., Shulte-Ladbeck, R., Slosar, A., Smith, D. S., Smoot, G., Springer, W., Stril, A., Szalay, A. S., Tao, C., Tarle, G., Taylor, E., Tilquin, A., Tinker, J., Valdes, F., Wang, J., Wang, T., Weaver, B. A., Weinberg, D., White, M., Wood-Vasey, M., Yang, J., Yeche, X. Yang Ch, Zakamska, N., Zentner, A., Zhai, C., and Zhang, P.
Subjects: FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract: BigBOSS is a Stage IV ground-based dark energy experiment to study baryon acoustic oscillations (BAO) and the growth of structure with a wide-area galaxy and quasar redshift survey over 14,000 square degrees. It has been conditionally accepted by NOAO in response to a call for major new instrumentation and a high-impact science program for the 4-m Mayall telescope at Kitt Peak. The BigBOSS instrument is a robotically-actuated, fiber-fed spectrograph capable of taking 5000 simultaneous spectra over a wavelength range from 340 nm to 1060 nm, with a resolution R = 3000-4800. Using data from imaging surveys that are already underway, spectroscopic targets are selected that trace the underlying dark matter distribution. In particular, targets include luminous red galaxies (LRGs) up to z = 1.0, extending the BOSS LRG survey in both redshift and survey area. To probe the universe out to even higher redshift, BigBOSS will target bright [OII] emission line galaxies (ELGs) up to z = 1.7. In total, 20 million galaxy redshifts are obtained to measure the BAO feature, trace the matter power spectrum at smaller scales, and detect redshift space distortions. BigBOSS will provide additional constraints on early dark energy and on the curvature of the universe by measuring the Ly-alpha forest in the spectra of over 600,000 2.2 < z < 3.5 quasars. BigBOSS galaxy BAO measurements combined with an analysis of the broadband power, including the Ly-alpha forest in BigBOSS quasar spectra, achieves a FOM of 395 with Planck plus Stage III priors. This FOM is based on conservative assumptions for the analysis of broad band power (kmax = 0.15), and could grow to over 600 if current work allows us to push the analysis to higher wave numbers (kmax = 0.3). BigBOSS will also place constraints on theories of modified gravity and inflation, and will measure the sum of neutrino masses to 0.024 eV accuracy., This report is based on the BigBOSS proposal submission to NOAO in October 2010, and reflects the project status at that time with minor updates

39. Evidence for major mergers of galaxies at 2 less than or similar to z < 4 in the VVDS and VUDS surveys

Author: Tasca, L. A. M., Le Fevre, O., Lopez-Sanjuan, C., Wang, P.-W., Cassata, P., Garilli, B., Ilbert, O., Le Brun, V., Lemaux, B. C., Maccagni, D., Tresse, L., Bardelli, S., Contini, T., Charlot, S., Cucciati, O., Fontana, A., Giavalisco, M., Kneib, J.-P., Salvato, M., Taniguchi, Y., Vergani, D., Zamorani, G., and Zucca, E.
Subjects: galaxies: high-redshift, galaxies: formation, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Context. The mass assembly of galaxies can proceed through different physical processes. Here we report on the spectroscopic identification of close physical pairs of galaxies at redshifts 2 less than or similar to z < 4 and discuss the impact of major mergers in building galaxies at these early cosmological times. Aims. We aim to identify and characterize close physical pairs of galaxies destined to merge and use their properties to infer the contribution of merging processes to the early mass assembly of galaxies. Methods. We searched for galaxy pairs with a transverse separation r(p)

40. Witnessing the build-up of the colour-density relation

Author: Cucciati, O., Iovino, A., Marinoni, C., Ilbert, O., Bardelli, S., Franzetti, P., Le Fevre, O., Pollo, A., Zamorani, G., Cappi, A., Guzzo, L., Mccracken, H. J., Meneux, B., Scaramella, R., Scodeggio, M., Tresse, L., Zucca, E., Bottini, D., Garilli, B., Le Brun, V., Maccagni, D., Picat, J. P., Vettolani, G., Zanichelli, A., Adami, C., Arnaboldi, M., Arnouts, S., Bolzonella, M., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Gavignaud, I., Marano, B., Mazure, A., Merighi, R., Paltani, S., Pello, R., Pozzetti, L., Radovich, M., Bondi, M., Bongiorno, A., Busarello, G., La Torre, S., Gregorini, L., Lamareille, F., Mathez, G., Mellier, Y., Paola Merluzzi, Ripepi, V., Rizzo, D., Temporin, G., Vergani, D., 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), and L.Tresse, S. Maurogordato and J. Tran Thanh Van
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We investigate the redshift and luminosity evolution of the galaxy colour-density relation using the data from the First Epoch VIMOS-VLT Deep Survey (VVDS) on scales of R=5 h^(-1)Mpc up to redshift z ~ 1.5. While at lower redshift we confirm the existence of a steep colour-density relation, with the fraction of the reddest(/bluest) galaxies of the same luminosity increasing(/decreasing) as a function of density, this trend progressively disappears in the highest redshift bins investigated.Our results suggest the existence of an epoch (more remote for brighter galaxies) characterized by the absence of the colour-density relation on the R=5 h^(-1)Mpc scales investigated. The rest frame u*-g' colour-magnitude diagram shows a bimodal pattern in both low and high density environments up to redshift z ~ 1.5. We find that the bimodal distribution is not universal but strongly depends upon environment. Both the colour-density and colour-magnitude-density relations, on the R=5 h^(-1)Mpc scales, appear to be a transient, cumulative product of genetic and environmental factors that have been operating over at least a period of 9 Gyr. These findings support an evolutionary scenario in which star formation/gas depletion processes are accelerated in more luminous objects and in high density environments: star formation activity is progressively shifting with cosmic time towards lower luminosity galaxies (downsizing), and out of high density environments., Comment: 6 pages, 3 figures, To appear in the proceedings of the XLIst Rencontres de Moriond, XXVIth Astrophysics Moriond Meeting: "From dark halos to light", Eds. L.Tresse, S. Maurogordato and J. Tran Thanh Van (Editions Frontieres)

41. Analogues of primeval galaxies two billion years after the Big Bang

Author: Amorín, R, Fontana, A, Pérez-Montero, E, Castellano, M, Guaita, L, Grazian, A, Fèvre, OL, Ribeiro, B, Schaerer, D, Tasca, LAM, Thomas, R, Bardelli, S, Cassarà, L, Cassata, P, Cimatti, A, Contini, T, Barros, SD, Garilli, B, Giavalisco, M, Hathi, N, Koekemoer, A, Le Brun, V, Lemaux, BC, Maccagni, D, Pentericci, L, Pforr, J, Talia, M, Tresse, L, Vanzella, E, Vergani, D, Zamorani, G, Zucca, E, and Merlin, E
Subjects: galaxies and clusters, 13. Climate action, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmology, Astrophysics::Galaxy Astrophysics
Abstract: Deep observations are revealing a growing number of young galaxies in the first billion years of cosmic time. Compared to typical galaxies at later times, they show more extreme emission-line properties, higher star formation rates, lower masses, and smaller sizes. However, their faintness precludes studies of their chemical abundances and ionization conditions, strongly limiting our understanding of the physics driving early galaxy build-up and metal enrichment. Here we study a rare population of ultraviolet-selected, low-luminosity galaxies at redshift 2.4 < z < 3.5 that exhibit all the rest-frame properties expected from primeval galaxies. These low-mass, highly compact systems are rapidly forming galaxies able to double their stellar mass in only a few tens of millions of years. They are characterized by very blue ultraviolet spectra with weak absorption features and bright nebular emission lines, which imply hard radiation fields from young hot massive stars. Their highly ionized gas phase has strongly sub-solar carbon and oxygen abundances, with metallicities more than a factor of two lower than that found in typical galaxies of similar mass and star formation rate at z≤2.5. These young galaxies reveal an early and short stage in the assembly of their galactic structures and their chemical evolution, a vigorous phase that is likely to be dominated by the effects of gas-rich mergers, accretion of metal-poor gas and strong outflows.

42. The VIMOS VLT Deep Survey: Public release of 1599 redshifts to IAB<=24 across the Chandra Deep Field South

Author: Le Fevre, O., Vettolani, G., Paltani, S., Laurence Tresse, Zamorani, G., Le Brun, V., Moreau, C., Vimos Vlt Deep Survey Team, 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), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: {This paper presents the VIMOS VLT Deep Survey around the Chandra Deep Field South (CDFS). We have measured 1599 new redshifts with VIMOS on the European Observatory Very Large Telescope - UT3, in an area 21x21.6 arcmin^2, including 784 redshifts in the Hubble Space Telescope - Advanced Camera for Surveys GOODS area. 30% of all objects with I_AB=24 have been observed independently of magnitude, indicating that the sample is purely magnitude limited. We have reached an unprecedented completeness level of 88% in terms of the ratio of secure measurements vs. observed objects, while 95% of all objects have a redshift measurement. A total of 1452 galaxies, 139 stars, 8 QSOs have a redshift identification, 141 of these being unsecure measurements. The redshift distribution down to I_AB=24 is peaked at a median redshift z=0.73, with a significant high redshift tail extending up to ~4. Several high density peaks in the distribution of galaxies are identified. In particular, the strong peak at z=0.735 contains more than 130 galaxies in a velocity range +/-2000 km/s distributed all across the transverse ~20 h^-1 Mpc of the survey. We are releasing all redshifts to the community, along with the cross identification with HST-ACS GOODS sources on the CENCOS database environment http://cencosw.oamp.fr., Comment: 9 pages, 8 figures (figure 8 is too big to be compressed for astro-ph), submitted to Astronomy and Astrophysics. The uncompressed version can be found on cencosw.oamp.fr

43. Galaxy luminosity function per morphological type up to z=1.2

Author: Ilbert, O., Lauger, S., Tresse, L., Buat, V., Arnout, S., Le Fevre, O., Burgarella, D., Zucca, E., Bardelli, S., Zamorani, G., Bottini, D., Garilli, B., Le Brun, V., Maccagni, D., Picat, J. -P, Scaramella, R., Scodeggio, M., Vettolani, G., Zanichelli, A., Adami, C., Arnaboldi, M., Bolzonella, M., Cappi, A., Charlot, S., Contini, T., Foucaud, S., Franzetti, P., Gavignaud, I., Guzzo, L., Iovino, A., Mccracken, H. J., Marano, B., Marinoni, C., Mathez, G., Mazure, A., Meneux, B., Roberto Merighi, Paltani, S., Pello, R., Pollo, A., Pozzetti, L., Radovich, M., Bondi, M., Bongiorno, A., Busarello, G., Ciliegi, P., Mellier, Y., Merluzzi, P., Ripepi, V., Rizzo, D., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We have computed the evolution of the rest-frame B-band luminosity function (LF) for bulge and disk-dominated galaxies since z=1.2. We use a sample of 605 spectroscopic redshifts with I_{AB}0.9 and bright galaxies showing a strongly decreasing LF slope \alpha=+0.55 \pm 0.21, and 32% of blue (B-I)_{AB}, Comment: 9 pages, 4 figures, 2 tables, accepted for publication in Astronomy and Astrophysics

44. The VIMOS Ultra Deep Survey: Ly$\alpha$ Emission and Stellar Populations of Star-Forming Galaxies at 2〈z〈2.5

Author: Hathi, Nimish P., Le Fèvre, O., Ilbert, O., Cassata, P., Tasca, L. A. M., Lemaux, B. C., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zamorani, G., Zucca, E., Amorín, R., Bardelli, S., Cassarà, L. P., Castellano, M., Cimatti, A., Cucciati, O., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Guaita, L., Koekemoer, A., Paltani, S., Pforr, J., Ribeiro, B., Schaerer, D., Marco Scodeggio, Sommariva, V., Talia, M., Tresse, L., Vergani, D., Capak, P., Charlot, S., Contini, T., Cuby, J. G., La Torre, S., Dunlop, J., Fotopoulou, S., López-Sanjuan, C., Mellier, Y., Salvato, M., Scoville, N., Taniguchi, Y., Wang, P. W., 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), AUTRES, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Oncology Institute of Southern Switzerland, INAF - Osservatorio Astronomico di Bologna (OABO), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), Space Telescope Science Institute (STSci), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), Institute of cosmology and gravitation, University of Portsmouth, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF- Milano, INAF - Osservatorio Astrofisico di Arcetri (OAA), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, SUPA, Institute for Astronomy, University of Edinburgh, Aristotle University of Thessaloniki, 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 Extraterrestrische Physik (MPE), Excellence Cluster Universe, excellence cluster centre, California Institute of Technology (CALTECH), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), University of Geneva [Switzerland], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: The aim of this paper is to investigate spectral and photometric properties of 854 faint ($i_{AB}$$0\AA), and Ly$\alpha$ emitters (LAEs; EW$\ge$20\AA). The fraction of LAEs at these redshifts is $\sim$10%, which is consistent with previous observations. We compared best-fit SED-estimated stellar parameters of the SFG$_{\rm N}$, SFG$_{\rm L}$ and LAE samples. For the luminosities probed here ($\sim$L$^*$), we find that galaxies with and without Ly$\alpha$ in emission have small but significant differences in their SED-based properties. We find that LAEs have less dust, and lower star-formation rates (SFR) compared to non-LAEs. We also find that LAEs are less massive compared to non-LAEs, though the difference is smaller and less significant compared to the SFR and E$_{\rm s}$(B-V). [abridged], Comment: Accepted for publication in A&A, 19 pages, 10 figures, 1 table
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45. The zCOSMOS redshift survey : Influence of luminosity, mass and environment on the galaxy merger rate

Author: Ravel, L., Kampczyk, P., Le Fèvre, O., Lilly, S. J., Tasca, L., Tresse, L., Lopez-Sanjuan, C., Bolzonella, M., Kovac, K., Abbas, U., Bardelli, S., Bongiorno, A., Caputi, K., Contini, T., Coppa, G., Cucciati, O., La Torre, S., Dunlop, J. S., Franzetti, P., Garilli, B., Iovino, A., Kneib, J. -P, Koekemoer, A. M., Knobel, C., Lamareille, F., Le Borgne, J. -F, Le Brun, V., Leauthaud, A., Maier, C., Mainieri, V., Mignoli, M., Pello, R., Peng, Y., Perez Montero, E., Ricciardelli, E., Scodeggio, M., Silverman, J. D., Tanaka, M., Vergani, D., Zamorani, G., Zucca, E., Bottini, D., Cappi, A., Carollo, C. M., Cassata, P., Cimatti, A., Marco Fumana, Guzzo, L., Maccagni, D., Marinoni, C., Mccracken, H. J., Memeo, P., Meneux, B., Oesch, P., Porciani, C., Pozzetti, L., Renzini, A., Scaramella, R., Scarlata, C., 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: Astrophysics - Cosmology and Extragalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, [INFO]Computer Science [cs], Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The contribution of major mergers to galaxy mass assembly along cosmic time is an important ingredient to the galaxy evolution scenario. We aim to measure the evolution of the merger rate for both luminosity/mass selected galaxy samples and investigate its dependence with the local environment. We use a sample of 10644 spectroscopically observed galaxies from the zCOSMOS redshift survey to identify pairs of galaxies destined to merge, using only pairs for which the velocity difference and projected separation of both components with a confirmed spectroscopic redshift indicate a high probability of merging. We have identified 263 spectroscopically confirmed pairs with r_p^{max} = 100 h^{-1} kpc. We find that the density of mergers depends on luminosity/mass, being higher for fainter/less massive galaxies, while the number of mergers a galaxy will experience does not depends significantly on its intrinsic luminosity but rather on its stellar mass. We find that the pair fraction and merger rate increase with local galaxy density, a property observed up to redshift z=1. We find that the dependence of the merger rate on the luminosity or mass of galaxies is already present up to redshifts z=1, and that the evolution of the volumetric merger rate of bright (massive) galaxies is relatively flat with redshift with a mean value of 3*10^{-4} (8*10^{-5} respectively) mergers h^3 Mpc^{-3} Gyr^{-1}. The dependence of the merger rate with environment indicates that dense environments favors major merger events as can be expected from the hierarchical scenario. The environment therefore has a direct impact in shapping-up the mass function and its evolution therefore plays an important role on the mass growth of galaxies along cosmic time., Comment: submitted to A&A, 17 pages, 12 figures

46. Less and more IGM-transmitted galaxies from z ∼ 2.7 to z ∼ 6 from VANDELS and VUDS

Author: E. Zucca, J. P. U. Fynbo, Margherita Talia, Ricardo Amorín, Anton M. Koekemoer, Y. Khusanova, Stefano Cristiani, Pascale Hibon, Laura Pentericci, Marco Castellano, F. Mannucci, Daniel Schaerer, S. Bardelli, V. Le Brun, Andrea Cimatti, R. Thomas, B. Garilli, M. Franco, O. Le Fevre, Adriana Gargiulo, Giovanni Cresci, Fabio Fontanot, Nimish P. Hathi, Brian C. Lemaux, G. Zamorani, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Thomas R., Pentericci L., Le Fevre O., Koekemoer A.M., Castellano M., Cimatti A., Fontanot F., Gargiulo A., Garilli B., Talia M., Amorin R., Bardelli S., Cristiani S., Cresci G., Franco M., Fynbo J.P.U., Hathi N.P., Hibon P., Khusanova Y., Le Brun V., Lemaux B.C., Mannucci F., Schaerer D., Zamorani G., and Zucca E.
Subjects: Physics, 0303 health sciences, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology: miscellaneou, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, 03 medical and health sciences, Space and Planetary Science, galaxies: high-redshift, Intergalactic medium, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, intergalactic medium, cosmology: miscellaneous, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 030304 developmental biology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aim. Our aim is to analyse the variance of the Inter-Galactic Medium transmission (IGM) by studying this parameter in the rest-frame UV spectra of a large sample of high redshift galaxies. Method. We make use of the VIMOS Ultra Deep Survey and the VANDELS public survey to have an insight into the far UV spectrum of $2.7, Comment: Accepted for publication on A&A
Published: 2021
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47. UV and Ly$\alpha$ luminosity functions of galaxies and star formation rate density at the end of HI reionization from the VIMOS UltraDeep Survey (VUDS)

Author: Paolo Cassata, F. Marchi, Marco Castellano, Laurence Tresse, Nimish P. Hathi, O. Cucciati, Janine Pforr, O. Le Fevre, Daniel Schaerer, Anton M. Koekemoer, Mauro Giavalisco, L. A. M. Tasca, Y. Khusanova, Ricardo Amorín, S. Bardelli, Laura Pentericci, R. Thomas, B. Ribeiro, D. Maccagni, Brian C. Lemaux, Daniela Vergani, Letizia P. Cassarà, E. Zucca, G. Zamorani, Andrea Cimatti, V. Le Brun, O. Ilbert, B. Garilli, 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 Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Khusanova Y., Le Fevre O., Cassata P., Cucciati O., Lemaux B.C., Tasca L.A.M., Thomas R., Garilli B., Le Brun V., MacCagni D., Pentericci L., Zamorani G., Amorin R., Bardelli S., Castellano M., Cassara L.P., Cimatti A., Giavalisco M., Hathi N.P., Ilbert O., Koekemoer A.M., Marchi F., Pforr J., Ribeiro B., Schaerer D., Tresse L., Vergani D., and Zucca E.
Subjects: galaxies: high-redshift, galaxies: evolution, galaxies: formation, galaxies: star formation, dark ages, reionization, first stars, galaxies: luminosity function, mass function, Population, first stars, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, dark ages, education, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, education.field_of_study, 010308 nuclear & particles physics, Galaxies: luminosity function, mass function, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Dark ages, reionization, first star, galaxies: luminosity function, Space and Planetary Science, mass function, reionization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We establish a robust statistical description of the star-forming galaxy population at the end of cosmic HI reionization ($5.0\le{}z\le6.6$) from a large sample of 52 galaxies with spectroscopically confirmed redshifts from the VIMOS UltraDeep Survey. We identify galaxies with Ly$\alpha$ either in absorption or in emission, at variance with most spectroscopic samples in the literature where Ly$\alpha$ emitters dominate. We find that star-forming galaxies at these redshifts are distributed along a main sequence in the stellar mass vs. SFR plane. We report a flat evolution of the sSFR(z) in 32. The bright end of the Ly$\alpha$ luminosity function has a high number density, indicating a significant star formation activity concentrated in the brightest Ly$\alpha$ emitters (LAE) at these redshifts. LAE with EW>25\AA ~contribute to about 75\% of the total UV-derived SFRD. While our analysis favors a low dust content in 5.0, Comment: 27 pages, submitted to A&A
Published: 2020
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48. The VIMOS Public Extragalactic Redshift Survey (VIPERS): Environment-size relation of massive passive galaxies at 0.5 ≤ z ≤ 0.8

Author: P. Franzetti, O. Cucciati, S. de la Torre, A. Zanichelli, Alexander Fritz, John A. Peacock, C. Adami, Federico Marulli, S. Arnouts, A. Gargiulo, Katarzyna Małek, Ummi Abbas, Enzo Branchini, M. Polletta, A. Cappi, M. Bolzonella, A. Iovino, B. Garilli, Luigi Guzzo, Thibaud Moutard, Chris P. Haines, A. J. Hawken, O. Le Fèvre, Agnieszka Pollo, Jean Coupon, Rita Tojeiro, Lidia Tasca, V. Le Brun, O. Ilbert, D. Bottini, M. Scodeggio, Benjamin R. Granett, G. De Lucia, Julien Bel, J. Krywult, D. Vergani, D. Maccagni, G. Zamorani, Lauro Moscardini, 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 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), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Saint Mary's University [Halifax], Aix Marseille Université (AMU), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), CPT - E3 Cosmologie, Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Gargiulo, A., Cucciati, O., Garilli, B., Scodeggio, M., Bolzonella, M., Zamorani, G., De Lucia, G., Krywult, J., Guzzo, L., Granett, B. R., de la Torre, S., Abbas, U., Adami, C., Arnouts, S., Bottini, D., Cappi, A., Franzetti, P., Fritz, A., Haines, C., Hawken, A. J., Iovino, A., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Moutard, T., Polletta, M., Pollo, A., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Bel, J., Branchini, E., Coupon, J., Ilbert, O., Moscardini, L., Peacock, J. A., University of St Andrews. School of Physics and Astronomy, 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 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), ITA, GBR, FRA, and POL
Subjects: Stellar mass, formation [galaxies], Population, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Satellite galaxy, QB Astronomy, galaxies: formation, education, 010303 astronomy & astrophysics, QC, evolution [galaxies], Astrophysics::Galaxy Astrophysics, QB, Physics, education.field_of_study, 010308 nuclear & particles physics, Sigma, Astronomy and Astrophysics, 3rd-DAS, Redshift survey, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Accretion (astrophysics), QC Physics, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract: We use the statistics of the VIPERS survey to investigate the relation between the surface mean stellar mass density Sigma=Mstar/(2*pi*Re^2) of massive passive galaxies (MPGs, Mstar>10^11 Msun) and their environment in the redshift range 0.52*10^11 Msun, we find an excess of MPGs with low Sigma and a deficit of high-Sigma MPGs in the densest regions wrt other environments. We interpret this result as due to the migration of some high-Sigma MPGs (0.8 migrate to the MPG population. Here, we investigate the Sigma-delta relation of MSFGs at z>0.8 and find that it is consistent within 1 sigma with that of low-Sigma MPGs at z0.8 are consistent in terms of number and environment with being the progenitors of low-Sigma MPGs at z, Comment: 12 pages, accepted for publication in A&A
Published: 2019
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49. The progeny of a Cosmic Titan: a massive multi-component proto-supercluster in formation at $z=2.45$ in VUDS

Author: Letizia P. Cassarà, V. Le Brun, Paolo Cassata, Eros Vanzella, Mara Salvato, Daniela Vergani, O. Le Fèvre, Nimish P. Hathi, L. Pentericci, E. Zucca, Anton M. Koekemoer, L. M. Lubin, D. Maccagni, Janine Pforr, Ricardo Amorín, Lidia Tasca, Bianca Garilli, Andrea Cimatti, Olga Cucciati, K. G. Lee, Brian C. Lemaux, S. Bardelli, Margherita Talia, G. Zamorani, R. C. Thomas, 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), Cucciati, O., Lemaux, B.C., Zamorani, G., Le Fèvre, O., Tasca, L.A.M., Hathi, N.P., Lee, K.-G., Bardelli, S., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Lubin, L.M., Amorin, R., Cassarà, L.P., Cimatti, A., Talia, M., Vergani, D., Koekemoer, A., Pforr, J., Salvato, M., and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Cosmology: observation, 01 natural sciences, Supercluster, galaxies: high-redshift, 0103 physical sciences, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Line-of-sight, 010308 nuclear & particles physics, Velocity dispersion, Astronomy and Astrophysics, Virial mass, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cosmology: observations, Galaxies: clusters: general, Galaxies: high-redshift, Large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: [Abridged] We unveil the complex shape of a proto-supercluster at z~2.45 in the COSMOS field using the spectroscopic redshifts of the VIMOS Ultra-Deep Survey (VUDS), complemented by the zCOSMOS-Deep sample and high-quality photometric redshifts. The method relies on a 2D Voronoi tessellation in overlapping redshift slices that is converted into a 3D density field. The galaxy distribution is constructed using a statistical treatment of spectroscopic and photometric redshifts. We identify a proto-supercluster, dubbed "Hyperion" for its immense size and mass, which extends over a volume of ~60x60x150 comoving Mpc^3 and has an estimated total mass of ~4.8x 10^15 M_sun. This immensely complex structure contains at least 7 density peaks within 2.4 < z < 2.5, connected by filaments. Based on the peaks average matter density, we estimate their total mass, M_tot, and find a range of masses from ~0.1x10^14 M_sun to ~2.7x10^14 M_sun. By using spectroscopic members of each peak, we obtain the velocity dispersion of the galaxies in the peaks, and then their virial mass M_vir (under the strong assumption that they are virialised). The agreement between M_vir and M_tot is surprisingly good, considering that almost all the peaks are probably not yet virialised. According to the spherical collapse model, the peaks have already started or are about to start collapsing, and they are all predicted to be virialised by redshift z~0.8-1.6. We finally perform a careful comparison with the literature, given that smaller components of this proto-supercluster had previously been identified using heterogeneous galaxy samples. With VUDS, we obtain a panoramic view of this large structure, that encompasses, connects, and considerably expands in a homogeneous way on all previous detections of the various sub-components. This provides us the unique possibility to study a rich supercluster in formation., 22 pages, 13 figures, accepted to be published in A&A, very minor corrections after language editing
Published: 2018
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50. The VIMOS Public Extragalactic Redshift Survey (VIPERS). An unbiased estimate of the growth rate of structure at ⟨z⟩ = 0.85 using the clustering of luminous blue galaxies

Author: O. Cucciati, S. de la Torre, Alexander Fritz, Jean Coupon, O. Le Fèvre, Katarzyna Małek, M. Polletta, F. G. Mohammad, P. Franzetti, A. Zanichelli, T. Moutard, John A. Peacock, Ummi Abbas, I. Davidzon, J. Krywult, B. Garilli, A. Iovino, Federico Marulli, G. De Lucia, M. Bolzonella, Rita Tojeiro, Enzo Branchini, D. Maccagni, A. Cappi, C. Adami, Luigi Guzzo, Lauro Moscardini, Agnieszka Pollo, L. A. M. Tasca, B. R. Granett, S. Arnouts, M. Scodeggio, D. Vergani, Julien Bel, V. Le Brun, O. Ilbert, D. Bottini, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-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), 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), Aix Marseille Université (AMU), 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), 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 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), 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 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 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), Centre de Physique Théorique - UMR 7332 ( CPT ), Aix Marseille Université ( AMU ) -Université de Toulon ( UTLN ) -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'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( 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 ), Aix Marseille Université ( AMU ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Mohammad, F. G., Granett, B. R., Guzzo, L., Bel, J., Branchini, E., De La Torre, S., Moscardini, L., Peacock, J. A., Bolzonella, M., Garilli, B., Scodeggio, M., Abbas, U., Adami, C., Bottini, D., Cappi, A., Cucciati, O., Davidzon, I., Franzetti, P., Fritz, A., Iovino, A., Krywult, J., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Polletta, M., Pollo, A., Tasca, L. A. M., Tojeiro, R., Vergani, D., Zanichelli, A., Arnouts, S., Coupon, J., De Lucia, G., Ilbert, O., Moutard, T., Mohammad, F.G., Granett, B.R., Peacock, J.A., MacCagni, D., Tasca, L.A.M., ARAG - AREA FINANZA E PARTECIPATE, DIP. DI ASTRONOMIA, DIPARTIMENTO DI FISICA E ASTRONOMIA 'AUGUSTO RIGHI', Da definire, and AREA MIN. 02 - Scienze fisiche
Subjects: statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Statistic [Galaxies], Large-scale structure of Universe, media_common.quotation_subject, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), 01 natural sciences, Cosmology, Spectral line, galaxies: high-redshift, 0103 physical sciences, Galaxies: Statistic, Observation [Cosmology], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: statistics, media_common, Physics, Cosmology: Observations, Galaxies: High-redshift, Galaxies: Statistics, Astronomy and Astrophysics, Space and Planetary Science, 010308 nuclear & particles physics, Astronomy and Astrophysic, Redshift survey, Galaxy, Universe, Redshift, observations [cosmology], Cosmology: Observation, cosmology: observations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], High-redshift [Galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use the VIPERS final data release to investigate the performance of colour-selected populations of galaxies as tracers of linear large-scale motions. We empirically select volume-limited samples of blue and red galaxies as to minimise the systematic error on the estimate of the growth rate $f\sigma_8$ from the anisotropy of the two-point correlation function. To this end, rather than rigidly splitting the sample into two colour classes we define the red/blue fractional contribution of each object through a weight based on the $(U-V)$ colour distribution. Using mock surveys that are designed to reproduce the observed properties of VIPERS galaxies, we find the systematic error in recovering the fiducial value of $f\sigma_8$ to be minimized when using a volume-limited sample of luminous blue galaxies. We model non-linear corrections via the Scoccimarro extension of the Kaiser model, finding systematic errors on $f\sigma_8$ of below $1-2\%$, using scales as small as 5 $h^{-1}\mathrm{Mpc}$. We interpret this result as indicating that selection of luminous blue galaxies maximises the fraction that are central objects in their dark matter haloes; this in turn minimises the contribution to the measured $\xi(r_p,\pi)$ from the 1-halo term, which is dominated by non-linear motions. The gain is inferior if one uses the full magnitude-limited sample of blue objects, consistent with the presence of a significant fraction of blue, fainter satellites dominated by non-streaming, orbital velocities. We measure a value of $f\sigma_8=0.45 \pm 0.11$ over the single redshift range $0.6\le z\le 1.0$, corresponding to an effective redshift for the blue galaxies $\left=0.85$. Including in the likelihood the potential extra information contained in the blue-red galaxy cross-correlation function does not lead to an appreciable improvement in the error bars, while it increases the systematic error., Comment: 20 pages, 21 figures, accepted for publication in A&A
Published: 2018
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