Author: "J. P. Picat" / Topic: galaxy - Searchworks@Jio Institute Digital Library Search Results

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43 results on '"J. P. Picat"'

1. VVDS-SWIRE

Author: S. Temporin, D. Maccagni, F. Lamareille, Duncan Farrah, Alain Mazure, C. J. Walcher, Paolo Ciliegi, Christian Marinoni, B. Garilli, V. Le Brun, O. Ilbert, D. Vergani, J. P. Picat, Fan Fang, L. Tresse, T. Contini, Angela Bongiorno, Jarle Brinchmann, E. Zucca, P. Franzetti, S. Paltani, Roberto Scaramella, R. Merighi, Stephane Arnouts, R. Pello, O. Le Fevre, Lucia Pozzetti, G. Zamorani, A. Zanichelli, Stéphane Charlot, M. Bondi, Mario Radovich, S. J. Oliver, H. J. McCracken, David L. Shupe, O. Cucciati, Carol J. Lonsdale, S. de la Torre, Yannick Mellier, D. Bottini, Bruno Marano, C. Adami, A. Pollo, I. Gavignaud, S. Bardelli, Paola Merluzzi, Luigi Guzzo, M. Bolzonella, I. Waddington, Marco Scodeggio, G. Vettolani, A. Iovino, Sylvie Foucaud, Jason Surace, B. Meneux, A. Cappi, 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, Department of Astronomy, Cornell University, Infrared Processing Analysis Center, California Institute of Technology (IPAC), University of Sussex, Observatoire Astronomique de l'Université de Genève, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Spitzer Science Center, California Institute of Technology (SSC), 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), IRA-INAF, Bologna, INAF-Osservatorio Astronomico di Bologna (OABO), Max-Planck-Institut für Astrophysik (MPA), 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), School of Physics and Astronomy, University of Nottingham, Astrophysikalisches Institut Potsdam (AIP), Institute for Astronomy, University of Hawaii, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-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), INTEGRAL Science Data Centre, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), and Centro de Astrofisica da Universidade do Porto (CAUP)
Subjects: Physics, Star formation, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Correlation function (astronomy), Galaxy, Redshift, Luminosity, Photometry (optics), Stars, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cluster analysis, Astrophysics::Galaxy Astrophysics
Abstract: International audience; 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 mu 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 mu m and 4.5 mu 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 mu m and 4.5 mu 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 mu m and a mean value of r0 ~= 4.4±0.5 h-1 Mpc for the galaxies selected at 4.5 mu 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 mum 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
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2. The VIMOS-VLT deep survey

Author: J. P. Picat, Stéphane Charlot, O. Cucciati, C. Adami, T. Contini, M. Bolzonella, Jarle Brinchmann, D. Bottini, Luigi Guzzo, C. J. Walcher, A. Pollo, I. Gavignaud, E. Zucca, A. Iovino, B. Meneux, S. Bardelli, Sylvie Foucaud, P. Franzetti, A. Zanichelli, Paolo Ciliegi, Marco Scodeggio, H. J. McCracken, A. Cappi, O. Le Fevre, G. Zamorani, F. Lamareille, R. Pello, D. Maccagni, Roberto Scaramella, Stéphane Paltani, A. Mazure, V. Le Brun, O. Ilbert, R. Merighi, Mario Radovich, Bruno Marano, Stephane Arnouts, B. Garilli, Lucia Pozzetti, L. Tresse, G. Vettolani, M. Arnaboldi, Christian Marinoni, D. Vergani, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), INAF-Osservatorio Astronomico di Brera, 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, University of Hawaii, INAF-Osservatorio Astronomico di Bologna (OABO), 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), Centro de Astrofisica da Universidade do Porto (CAUP), 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), Istituto di Radioastronomia, Bologna, School of Physics and Astronomy, University of Nottingham, Astrophysikalisches Institut Potsdam (AIP), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), INTEGRAL Science Data Centre, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Authors: Franzetti P., Scodeggio M., Garilli B., Vergani D., Maccagni D., Guzzo L., Tresse L., Ilbert O., Lamareille F., Contini T., Le Fèvre O., Zamorani G., Brinchmann J., Charlot S., Bottini D., Le Brun V., Picat J. P., Scaramella R., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Ciliegi P., Foucaud S., Gavignaud I., Iovino A., McCracken H. J., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Pozzetti L., Radovich M., Zucca E., Cucciati O., and Walcher C. J.
Subjects: GALAXIES: EVOLUTION, Physics, Astrophysics (astro-ph), COSMOLOGY: OBSERVATIONS, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Rest frame, Stellar classification, Redshift, Galaxy, Bimodality, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], VIMOS-VLT Deep Survey, Equivalent width, Astrophysics::Galaxy Astrophysics
Abstract: In this paper we discuss the mix of star-forming and passive galaxies up to z~2, based on the first epoch VIMOS-VLT Deep Survey (VVDS) data.In agreement with previous works we find that the galaxy rest-frame color distribution follows a bimodal distribution at z, 15 pages, 10 figures, 2 tables, revised version accepted for publication on A&A
Published: 2007
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3. A deep wide survey of faint low surface brightness galaxies in the direction of the Coma cluster of galaxies

Author: Melville P. Ulmer, S. Kasun, Roser Pello, Christopher J. Conselice, Michael D. Gregg, J. P. Picat, C. Adami, Florence Durret, R. Scheidegger, A. Mazure, M. J. West, arXiv, Import, 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), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Services communs OMP (UMS 831), 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), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy, Northwestern University, Evanston, Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Department of Physics and Astronomy, University of Hawaii, California Institute of Technology, Department of Astronomy (CALTECH), Department of Physics, Le Conte Hall, University of California, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), 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), 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: Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Coma (optics), Astrophysics, 01 natural sciences, Galaxy, Redshift, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU]Sciences of the Universe [physics], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, 0103 physical sciences, Magnitude (astronomy), Coma Cluster, Surface brightness, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics
Abstract: We report on a search for faint (R total magnitude fainter than 21) and low surface brightness galaxies (R central surface brightness fainter than ~24) (fLSBs) in a 0.72x0.82 deg2 area centered on the Coma cluster. We analyzed deep B and R band CCD imaging obtained using the CFH12K camera at CFHT and found 735 fLSBs. The total B magnitudes, at the Coma cluster redshift, range from -13 to -9 with B central surface brightness as faint as 27 mag/arcsec2. Using empty field comparisons, we show that most of these fLSBs are probably inside the Coma cluster. We present the results of comparing the projected fLSB distributions with the distributions of normal galaxies and with known X-ray over densities. We also investigate their projected distribution relative to their location in the color magnitude relation. Colors of fLSBs vary between B-R~0.8 and ~1.4 for 2/3 of the sample and this part is consistent with the known CMR red-sequence for bright (R, To be published in A&A, 3 jpeg figures, data and full resolution article can be retrieved from http://cencosw.oamp.fr/. Updated CFHT ackowledgements
Published: 2006
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4. The VIMOS VLT deep survey

Author: O. Le Fèvre, G. Vettolani, B. Garilli, L. Tresse, D. Bottini, V. Le Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, A. Zanichelli, C. Adami, M. Arnaboldi, S. Arnouts, S. Bardelli, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, O. Ilbert, A. Iovino, H. J. McCracken, B. Marano, C. Marinoni, G. Mathez, A. Mazure, B. Meneux, R. Merighi, S. Paltani, R. Pellò, A. Pollo, L. Pozzetti, M. Radovich, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, G. Busarello, F. Lamareille, Y. Mellier, P. Merluzzi, V. Ripepi, and D. Rizzo
Subjects: Physics, education.field_of_study, 010308 nuclear & particles physics, Population, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Apparent magnitude, Space and Planetary Science, 0103 physical sciences, Magnitude (astronomy), Galaxy formation and evolution, education, 010303 astronomy & astrophysics, Spectrograph, Data reduction
Abstract: This paper presents the ``First Epoch'' sample from the VIMOS VLT Deep Survey (VVDS). The VVDS goals, observations, data reduction with VIPGI, and redshift measurement with KBRED are discussed. Data have been obtained with the VIsible Multi Object Spectrograph (VIMOS) on the ESO-VLT UT3, allowing to observe ~600 slits simultaneously at R~230. A total of 11564 objects have been observed in the VVDS-02h and VVDS-CDFS Deep fields over a total area of 0.61deg^2, selected solely on the basis of apparent magnitude 17.5 1.4. The survey reaches a redshift measurement completeness of 78% overall (93% including less reliable objects), with a spatial sampling of the population of galaxies of 25% and ~30% in the VVDS-02h and VVDS-CDFS. The redshift accuracy measured from repeated observations with VIMOS and comparison to other surveys is ~276km/s. From this sample we present for the first time the redshift distribution of a magnitude limited spectroscopic sample down to IAB=24. The redshift distribution has a median of z=0.62, z=0.65, z=0.70, and z=0.76, for magnitude limited samples with IAB 23.5, probing the bright star forming population of galaxies. This sample provides an unprecedented dataset to study galaxy evolution over 90% of the life of the universe
Published: 2005
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5. The VIMOS VLT Deep Survey

Author: O. Le Fèvre, G. Vettolani, S. Paltani, L. Tresse, G. Zamorani, V. Le Brun, C. Moreau, D. Bottini, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, A. Cappi, S. Charlot, T. Contini, S. Foucaud, P. Franzetti, B. Garilli, I. Gavignaud, L. Guzzo, O. Ilbert, A. Iovino, H. J. McCracken, D. Mancini, B. Marano, C. Marinoni, G. Mathez, A. Mazure, B. Meneux, R. Merighi, R. Pellò, A. Pollo, L. Pozzetti, M. Radovich, E. Zucca, M. Arnaboldi, M. Bondi, A. Bongiorno, G. Busarello, P. Ciliegi, L. Gregorini, Y. Mellier, P. Merluzzi, V. Ripepi, and D. Rizzo
Subjects: QSOS, Physics, Very Large Telescope, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Advanced Camera for Surveys, Redshift, Galaxy, Stars, Space and Planetary Science, 0103 physical sciences, Magnitude (astronomy), Chandra Deep Field South, 010303 astronomy & 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 this http URL
Published: 2004
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6. The VIMOS VLT Deep Survey. The assembly history of the stellar mass in galaxies: from the young to the old universe

Author: O. Ilbert, R. Pello, E. Zucca, Sylvie Foucaud, Thierry Contini, F. Lamareille, C. Adami, I. Gavignaud, Paolo Ciliegi, Paola Merluzzi, P. Franzetti, A. Pollo, Roberto Scaramella, A. Mazure, S. Temporin, M. Radovich, Olga Cucciati, R. Merighi, Laurence Tresse, D. Maccagni, A. Zanichelli, Stéphane Arnouts, Bianca Garilli, V. Le Brun, Stéphane Paltani, A. Iovino, Angela Bongiorno, C. J. Walcher, S. Bardelli, J. P. Picat, Yannick Mellier, D. Bottini, B. Meneux, M. Scodeggio, A. Cappi, Micol Bolzonella, M. Bondi, Bruno Marano, Daniela Vergani, Luigi Guzzo, Christian Marinoni, Stephane Charlot, O. Le Fevre, Lucia Pozzetti, S. de la Torre, Jarle Brinchmann, G. Zamorani, Gianpaolo Vettolani, H. J. McCracken, L. Gregorini, INAF-Osservatorio Astronomico di Bologna (OABO), 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), 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)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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, Institute for Astronomy, University of Hawaii, Max-Planck-Institut für Astrophysik (MPA), 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), Centro de Astrofisica da Universidade do Porto (CAUP), Istituto di Radioastronomia, Bologna, School of Physics and Astronomy, University of Nottingham, Astrophysikalisches Institut Potsdam (AIP), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Astronomia, Università di Bologna, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), INTEGRAL Science Data Centre, Astronomical Observatory, Jagiellonia University, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Dipartimento di Fisica, Università di Bologna, AUTRES, Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), 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), Observatoire de Paris - Site de Paris (OP), 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), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Services communs OMP (UMS 831), Axe 1 : procédés céramiques, Science des Procédés Céramiques et de Traitements de Surface (SPCTS), Université de Limoges (UNILIM)-Ecole Nationale Supérieure de Céramique Industrielle (ENSCI)-Institut des Procédés Appliqués aux Matériaux (IPAM), Université de Limoges (UNILIM)-Université de Limoges (UNILIM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Limoges (UNILIM)-Ecole Nationale Supérieure de Céramique Industrielle (ENSCI)-Institut des Procédés Appliqués aux Matériaux (IPAM), Université de Limoges (UNILIM)-Université de Limoges (UNILIM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Beaussier, Catherine, 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), École normale supérieure - Paris (ENS Paris), L. Pozzetti, M. Bolzonella, F. Lamareille, G. Zamorani, P. Franzetti, O. Le Fèvre, A. Iovino, S. Temporin, O. Ilbert, S. Arnout, S. Charlot, J. Brinchmann, E. Zucca, L. Tresse, M. Scodeggio, L. Guzzo, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, J. P. Picat, R. Scaramella, G. Vettolani, A. Zanichelli, C. Adami, S. Bardelli, A. Cappi, P. Ciliegi, T. Contini, S. Foucaud, I. Gavignaud, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, S. Paltani, R. Pellò, A. Pollo, M. Radovich, M. Bondi, A. Bongiorno, O. Cucciati, S. de la Torre, L. Gregorini, Y. Mellier, P. Merluzzi, D. Vergani, and C. J. Walcher
Subjects: Stellar mass, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Redshift, Stars, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], VIMOS-VLT Deep Survey
Abstract: We present a detailed analysis of the Galaxy Stellar Mass Function of galaxies up to z=2.5 as obtained from the VVDS. We estimate the stellar mass from broad-band photometry using 2 different assumptions on the galaxy star formation history and show that the addition of secondary bursts to a continuous star formation history produces systematically higher (up to 40%) stellar masses. At low redshift (z=0.2) we find a substantial population of low-mass galaxies (10^8 Msun at z=1), and a mild mass-dependent average evolution (`mass-downsizing'). In particular our data are consistent with mild/negligible (6x10^10 Msun). For less massive systems the no-evolution scenario is excluded. A large fraction (>=50%) of massive galaxies have been already assembled and converted most of their gas into stars at z=1, ruling out the `dry mergers' as the major mechanism of their assembly history below z=1. This fraction decreases to 33% at z=2. Low-mass systems have decreased continuously in number and mass density (by a factor up to 4) from the present age to z=2, consistently with a prolonged mass assembly also at z, 20 pages with 12 encapsulated figures. Version accepted by A&A
Published: 2007

7. The VIMOS VLT Deep Survey: Evolution of the non-linear galaxy bias up to z=1.5

Author: C. Marinoni, O. Le Fèvre, B. Meneux, A. Iovino, A. Pollo, O. Ilbert, G. Zamorani, L. Guzzo, A. Mazure, R. Scaramella, A. Cappi, H. J. McCracken, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, J. P. Picat, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, J. Blaizot, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, B. Marano, G. Mathez, R. Merighi, S. Paltani, R. Pellò, L. Pozzetti, M. Radovich, E. Zucca, M. Bondi, A. Bongiorno, G. Busarello, S. Colombi, O. Cucciati, F. Lamareille, Y. Mellier, P. Merluzzi, V. Ripepi, D. Rizzo, 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), 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), Services communs OMP (UMS 831), 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), University of Oxford, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Departement de Radioastronomie Millimétrique (DEMIRM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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 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), University of Oxford [Oxford], Università di Bologna, Dipartimento di Astronomia, École normale supérieure - Paris (ENS Paris), C. Marinoni, O. Le Fèvre, B. Meneux, A. Iovino, A. Pollo, O. Ilbert, G. Zamorani, L. Guzzo, A. Mazure, R. Scaramella, A. Cappi, H. J. McCracken, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, J. P. Picat, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnout, S. Bardelli, J. Blaizot, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, B. Marano, G. Mathez, R. Merighi, S. Paltani, R. Pellò, L. Pozzetti, M. Radovich, E. Zucca, M. Bondi, A. Bongiorno, G. Busarello, S. Colombi, O. Cucciati, F. Lamareille, Y. Mellier, P. Merluzzi, V. Ripepi, and D. Rizzo
Subjects: FOS: Physical sciences, Probability density function, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 010303 astronomy & astrophysics, galaxies: statistics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Biasing, Function (mathematics), cosmology: large-scale structure of Universe, Galaxy, Redshift, galaxies: distances and redshift, Nonlinear system, Amplitude, Space and Planetary Science, galaxies: distances and redshifts, galaxies: evolution
Abstract: We present the first measurements of the Probability Distribution Function (PDF) of galaxy fluctuations in the VIMOS-VLT Deep Survey (VVDS) cone, covering 0.4x0.4 deg between 0.40.8; ii) the formation of bright galaxies is inhibited below a characteristic mass-overdensity threshold whose amplitude increases with redshift and luminosity; iii) the biasing function is non linear in all the redshift bins investigated with non-linear effects of the order of a few to 10% on scales >5Mpc., Comment: 30 pages, 17 figs, Accepted by A&A
Published: 2005
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8. Photometric redshifts as a tool for studying the Coma cluster galaxy populations

Author: Alain Mazure, J. P. Picat, R. Pello, M. P. Ulmer, Jean-Charles Cuillandre, C. Adami, O. Ilbert, F. Durret, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire 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), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), 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), NWU, Dearborn Observatory (NWU), Northwestern University Department of Physics and Astronomy, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Services communs OMP (UMS 831), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-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), 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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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, École normale supérieure - Paris (ENS Paris), and Beaussier, Catherine
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: clusters: individual: Coma, 0103 physical sciences, Cluster (physics), Coma Cluster, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Luminosity function (astronomy), Photometric redshift, Physics, Background subtraction, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Redshift, galaxies: luminosity function, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, mass function, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA]
Abstract: We investigate the Coma cluster galaxy luminosity function (GLF) at faint magnitudes, in particular in the u* band by applying photometric redshift techniques applied to deep u*, B, V, R, I images covering a region of ~1deg2 (R 24). Global and local GLFs in the B, V, R and I bands obtained with photometric redshift selection are consistent with our previous results based on a statistical background subtraction. In the area covered only by the u* image, the GLF was also derived after applying a statistical background subtraction. The GLF in the u* band shows an increase of the faint end slope towards the outer regions of the cluster (from alpha~1 in the cluster center to alpha~2 in the cluster periphery). This could be explained assuming a short burst of star formation in these galaxies when entering the cluster. The analysis of the multicolor type spatial distribution reveals that late type galaxies are distributed in clumps in the cluster outskirts, where X-ray substructures are also detected and where the GLF in the u* band is steeper., 14 pages, 2 figures in jpeg format, accepted in A&A
Published: 2008
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9. The VIMOS VLT Deep Survey. Testing the gravitational instability paradigm at z ~ 1

Author: C. Marinoni, L. Guzzo, A. Cappi, O. Le Fèvre, A. Mazure, B. Meneux, A. Pollo, A. Iovino, H. J. McCracken, R. Scaramella, S. de la Torre, J. M. Virey, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, J. P. Picat, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, O. Ilbert, F. Lamareille, B. Marano, G. Mathez, R. Merighi, S. Paltani, R. Pellò, L. Pozzetti, M. Radovich, D. Vergani, G. Zamorani, E. Zucca, U. Abbas, M. Bondi, A. Bongiorno, J. Brinchmann, A. Buzzi, O. Cucciati, L. de Ravel, L. Gregorini, Y. Mellier, P. Merluzzi, E. Perez-Montero, P. Taxil, S. Temporin, C. J. Walcher, 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), INAF- Milano, Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), 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), 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), 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), INAF - Osservatorio Astronomico di Bologna (OABO), European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto di Radioastronomia [Bologna] (IRA), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Bernardo, Elizabeth, AUTRES, 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), 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, Marinoni C., Guzzo L., Cappi A., Le Fèvre O., Mazure A., Meneux B., Pollo A., Iovino A., McCracken H. J., Scaramella R., de 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., de Ravel L., Gregorini L., Mellier Y., Merluzzi P., Perez-Montero E., Taxil P., Temporin S., and Walcher C. J.
Subjects: statistics [galaxies], Distribution (number theory), Field (physics), FOS: Physical sciences, Probability density function, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Measure (mathematics), GALASSIE, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], GRAVITAZIONE, galaxies: high-redshift, cosmology: theory, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: statistics, Physics, large-scale structure of Universe [cosmology], Galaxy: evolution, theory [cosmology], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, COSMOLOGIA, COSMOLOGIA OSSERVATIVA, cosmology: large-scale structure of Universe, Redshift, Galaxy, SURVEY, Space and Planetary Science, Skewness, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], evolution [galaxy], Perturbation theory (quantum mechanics), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], high-redshift [galaxies]
Abstract: We have reconstructed the three-dimensional density fluctuation maps to z ~ 1.5 using the distribution of galaxies observed in the VVDS-Deep survey. We use this overdensity field to measure the evolution of the probability distribution function and its lower-order moments over the redshift interval 0.7, Comment: 14 pages, 5 figures, A&A in Press
Published: 2008
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10. The VIMOS VLT Deep Survey. Tracing the galaxy stellar mass assembly history over the last 8 Gyr

Author: D. Vergani, M. Scodeggio, L. Pozzetti, A. Iovino, P. Franzetti, B. Garilli, G. Zamorani, D. Maccagni, F. Lamareille, O. Le Fèvre, S. Charlot, T. Contini, L. Guzzo, D. Bottini, V. Le Brun, J. P. Picat, R. Scaramella, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, A. Cappi, P. Ciliegi, S. Foucaud, I. Gavignaud, O. Ilbert, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, S. Paltani, R. Pellò, A. Pollo, M. Radovich, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, O. Cucciati, S. de la Torre, L. Gregorini, E. Perez-Montero, Y. Mellier, P. Merluzzi, S. Temporin, INAF- Milano, Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), 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), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), 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), INAF - Osservatorio Astronomico di Capodimonte (OAC), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), AUTRES, 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, Observatoire de Paris - Site de Paris (OP), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Services communs OMP (UMS 831), 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), European Southern Observatory (ESO), École normale supérieure - Paris (ENS Paris), 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), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Università di Bologna, Dipartimento di Astronomia, Universidade do Porto, Beaussier, Catherine, Vergani D., Scodeggio M., Pozzetti L., Iovino A., Franzetti P., Garilli B., Zamorani G., Maccagni D., Lamareille F., Le Fèvre O., Charlot S., Contini T., Guzzo L., Bottini D., Le Brun V., Picat J. P., Scaramella R., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Ciliegi P., Foucaud S., Gavignaud I., Ilbert O., McCracken H. J., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Radovich M., Zucca E., Bondi M., Bongiorno A., Brinchmann J., Cucciati O., de La Torre S., Gregorini L., Perez-Montero E., Mellier Y., Merluzzi P., and Temporin S.
Subjects: Stellar mass, formation [galaxies], Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: fundamental, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, GALASSIE, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, 0103 physical sciences, Galaxy formation and evolution, fundamental parameters [galaxies], Astrophysics::Solar and Stellar Astrophysics, galaxies: formation, education, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, parameters, SPETTROGRAFIA, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], EVOLUZIONE, 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Balmer series, Astronomy and Astrophysics, COSMOLOGIA, luminosity function, mass function [galaxies], Galaxy, Redshift, observations [cosmology], Stars, galaxies: luminosity function, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], mass function, cosmology: observations, symbols, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], galaxies: evolution
Abstract: We selected a mass-limited sample of 4048 objects from the VIMOS VLT Deep Survey in the redshift interval 0.5, Comment: Accepted for pubblication in A&A, 14 pages, 5 figures
Published: 2008
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11. The VIMOS VLT deep survey. The K-band follow-up in the 0226-04 field

Author: Daniela Vergani, M. Radovich, Sylvie Foucaud, O. Ilbert, Thierry Contini, C. J. Walcher, F. Lamareille, M. Bondi, R. Pello, G. Zamorani, I. Gavignaud, J. P. Picat, Stephane Charlot, H. J. McCracken, Angela Bongiorno, S. Temporin, D. Maccagni, V. Le Brun, M. Scodeggio, Stéphane Paltani, Laurence Tresse, B. Meneux, E. Zucca, A. Iovino, Giampaolo Vettolani, Yannick Mellier, Christian Marinoni, A. Cappi, Micol Bolzonella, Olga Cucciati, S. de la Torre, Lucia Pozzetti, D. Bottini, P. Franzetti, Luigi Guzzo, A. Zanichelli, Stéphane Arnouts, Jarle Brinchmann, O. Le Fevre, Paolo Ciliegi, A. Pollo, S. Bardelli, Bianca Garilli, Bruno Marano, Roberto Scaramella, A. Mazure, R. Merighi, C. Adami, Temporin S., Iovino A., Bolzonella M., McCracken H. J., Scodeggio M., Garilli B., Bottini D., Le Brun V., Le Fèvre O., Maccagni D., Picat J. P., Scaramella R., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Cappi A., Charlot S., Ciliegi P., Contini T., Cucciati O., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Ilbert O., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Pozzetti L., Radovich M., Vergani D., Zamorani G., Zucca E., Bondi M., Bongiorno A., Brinchmann J., de La Torre S., Lamareille F., Mellier Y., Walcher C. J., INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), 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 d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, European Southern Observatory (ESO), 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), INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto di Radioastronomia [Bologna] (IRA), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), 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, Università di Bologna, Dipartimento di Astronomia, and Universidade do Porto
Subjects: INFRAROSSO, Field (physics), REDSHIFT, FOS: Physical sciences, Astrophysics, 01 natural sciences, infrared: galaxies, GALASSIE, surveys, K band, 0103 physical sciences, Limit (mathematics), 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Epoch (reference date), Astrophysics (astro-ph), Vega, Astronomy and Astrophysics, COSMOLOGIA OSSERVATIVA, galaxies: general, cosmology: large-scale structure of Universe, Galaxy, Redshift, SURVEY, Space and Planetary Science, Magnitude (astronomy), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA]
Abstract: AIMS. We present a new Ks-band survey that represents a significant extension to the previous wide-field Ks-band imaging survey within the 0226-04 field of the VIMOS-VLT deep survey (VVDS). The new data add ~ 458 arcmin^2 to the previous imaging program, thus allowing us to cover a total contiguous area of ~ 600 arcmin^2 within this field. METHODS. Sources are identified both directly on the final K-band mosaic image and on the corresponding, deep chi^2-g'r'i' image from the CFHT Legacy Survey in order to reduce contamination while ensuring us the compilation of a truly K-selected catalogue down to the completeness limit of the Ks-band. The newly determined Ks-band magnitudes are used in combination with the ancillary multiwavelength data for the determination of accurate photometric redshifts. RESULTS. The final catalogue totals ~ 52000 sources, out of which ~ 4400 have a spectroscopic redshift from the VVDS first epoch survey. The catalogue is 90% complete down to K_Vega = 20.5 mag. We present K_s-band galaxy counts and angular correlation function measurements down to such magnitude limit. Our results are in good agreement with previously published work. We show that the use of K magnitudes in the determination of photometric redshifts significantly lowers the incidence of catastrophic errors. The data presented in this paper are publicly available through the CENCOS database., Comment: 16 pages, 17 figures, accepted for publication in A&A on 01/02/2008
Published: 2008
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12. The VIMOS-VLT Deep Survey (VVDS). The dependence of clustering on galaxy stellar mass at z ~ 1

Author: Sylvie Foucaud, J. Blaizot, F. Lamareille, E. Zucca, P. Franzetti, D. Bottini, Angela Bongiorno, Stephane Arnouts, Lucia Pozzetti, O. Le Fevre, O. Cucciati, D. Maccagni, G. Zamorani, B. Meneux, A. Cappi, S. de la Torre, G. De Lucia, T. Contini, Paolo Ciliegi, H. J. McCracken, M. Radovich, I. Gavignaud, R. Scaramella, C. Adami, A. Pollo, Luigi Guzzo, Marco Scodeggio, R. Pello, A. Iovino, S. Bardelli, U. Abbas, M. Bolzonella, V. Le Brun, O. Ilbert, J. P. Picat, L. Tresse, A. Zanichelli, Alain Mazure, G. Vettolani, C. Marinoni, D. Vergani, S. Paltani, R. Merighi, Bruno Marano, B. Garilli, Stéphane Charlot, Meneux B., Guzzo L., Garilli B., Le Fèvre O., Pollo A., Blaizot J., De Lucia G., Bolzonella M., Lamareille F., Pozzetti L., Cappi A., Iovino A., Marinoni C., McCracken H. J., de La Torre S., Bottini D., Le Brun V., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Abbas U., Adami C., Arnouts S., Bardelli S., Bongiorno A., Charlot S., Ciliegi P., Contini T., Cucciati O., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Marano B., Mazure A., Merighi R., Paltani S., Pellò R., Radovich M., Vergani D., Zamorani G., Zucca E., 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), INAF - Osservatorio Astronomico di Brera (OAB), INAF - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Capodimonte (OAC), Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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), University of Oxford, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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), Observatoire de Paris - Site de Paris (OP), 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), 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), Services communs OMP (UMS 831), INAF - Osservatorio Astronomico di Roma (OAR), Istituto di Radioastronomia [Bologna] (IRA), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Bologna (OAB), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Institute of Liver Studies, King's College Hospital (KCH), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), INAF-Osservatorio Astronomico di Brera (INAF-OAB), Astronomical Observatory, Jagiellonia University, INAF-Osservatorio Astronomico di Bologna (OABO), INAF-Osservatorio Astronomico di Brera, Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), IRA-INAF, Bologna, School of Physics and Astronomy, University of Nottingham, Astrophysikalisches Institut Potsdam (AIP), Institute for Astronomy, University of Hawaii, INTEGRAL Science Data Centre, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Oxford [Oxford], Università di Bologna, Dipartimento di Astronomia, 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, Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, 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), and Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI)
Subjects: Stellar mass, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Correlation function (astronomy), Measure (mathematics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], GALASSIE, surveys, Millennium Run, Astrophysics::Solar and Stellar Astrophysics, education, Astrophysics::Galaxy Astrophysics, evolution [galaxies], Physics, large-scale structure of Universe [cosmology], education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), GALSSIE, Astronomy and Astrophysics, COSMOLOGIA OSSERVATIVA, Galaxy, Redshift, observations [cosmology], SURVEY, MASSA, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Aims: We use the VVDS-Deep first-epoch data to measure the dependence of galaxy clustering on galaxy stellar mass, at z~0.85. Methods: We measure the projected correlation function wp(rp) for sub-samples with 0.510^9 Msun to r0 ~ 4.28 h^-1 Mpc for galaxies more massive than 10^10.5 Msun. At the same time, the slope increases from ~ 1.67 to ~ 2.28. A comparison of the observed wp(rp) to local measurements by the SDSS shows that the evolution is faster for objects less massive than ~10^10.5 Msun. This is interpreted as a higher dependence on redshift of the linear bias b_L for the more massive objects. While for the most massive galaxies b_L decreases from 1.5+/-0.2 at z~0.85 to 1.33+/-0.03 at z~0.15, the less massive population maintains a virtually constant value b_L~1.3. This result is in agreement with a scenario in which more massive galaxies formed at high redshift in the highest peaks of the density field, while less massive objects form at later epochs from the more general population of dark-matter halos., Comment: 13 pages, 10 figures, accepted in A&A
Published: 2008
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13. Geometrical tests of cosmological models. III. The cosmology-evolution diagram at z=1

Author: C. Marinoni, A. Saintonge, T. Contini, C. J. Walcher, R. Giovanelli, M. P. Haynes, K. L. Masters, O. Ilbert, A. Iovino, V. Le Brun, O. Le Fevre, A. Mazure, L. Tresse, J.-M. Virey, S. Bardelli, D. Bottini, B. Garilli, G. Guzzo, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, P. Taxil, G. Vettolani, A. Zanichelli, E. Zucca, 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), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, 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), Department of Biology, University of Washington [Seattle], 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), Center for Radiophysics and Space Research [Ithaca] (CRSR), Cornell University [New York], INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), AUTRES, INAF- Milano, INAF - Osservatorio Astronomico di Brera (OAB), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), 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), and 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)
Subjects: Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, galaxies: fundamental parameters, Redshift survey, Redshift, Galaxy, Space and Planetary Science, cosmology: observations, Dark energy, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], cosmology: cosmological parameters, galaxies: evolution
Abstract: The rotational velocity of distant galaxies, when interpreted as a size (luminosity) indicator, may be used as a tool to select high redshift standard rods (candles) and probe world models and galaxy evolution via the classical angular diameter-redshift or Hubble diagram tests. We implement the proposed testing strategy using a sample of 30 rotators spanning the redshift range 0.2, Comment: 14 pages and 11 figures. A&A in press
Published: 2008
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14. A test of the nature of cosmic acceleration using galaxy redshift distortions

Author: Sylvie Foucaud, F. Lamareille, E. Zucca, Alain Mazure, A. Pollo, M. Pierleoni, V. Le Brun, L. Tresse, O. Ilbert, S. Bardelli, O. Cucciati, S. de la Torre, Marco Scodeggio, C. Adami, M. Bolzonella, G. De Lucia, G. Zamorani, J. P. Picat, D. Bottini, Klaus Dolag, P. Memeo, A. Iovino, Enrique Perez-Montero, Gianpaolo Vettolani, Roberto Scaramella, B. Meneux, H. J. McCracken, R. Merighi, Thierry Contini, Lauro Moscardini, J. Blaizot, B. Garilli, I. Gavignaud, Bruno Marano, D. Maccagni, Stéphane Paltani, Stephane Charlot, A. Zanichelli, Luigi Guzzo, R. Pello, Enzo Branchini, A. Cappi, Angela Bongiorno, Mario Radovich, Christian Marinoni, D. Vergani, Stephane Arnouts, Lucia Pozzetti, Paolo Ciliegi, P. Franzetti, O. Le Fevre, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), 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), 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), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), INAF - Osservatorio Astronomico di Brera (OAB), INAF - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Capodimonte (OAC), Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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), University of Oxford, Services communs OMP (UMS 831), 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), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), INAF - Osservatorio Astronomico di Roma (OAR), Istituto di Radioastronomia [Bologna] (IRA), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Bologna (OAB), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Observatoire de Paris - Site de Paris (OP), 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), Institute of Liver Studies, King's College Hospital (KCH), Guzzo, L., Pierleoni, M., Meneux, B., Branchini, E, Le Fèvre, O., Marinoni, C., Garilli, B., Blaizot, J., De Lucia, G., Pollo, A., Mccracken, H. J., Bottini, D., Le Brun, V., Maccagni, D., Picat, J. P., Scaramella, R., Scodeggio, M., Tresse, L., Vettolani, G., Zanichelli, A., Adami, C., Arnouts, S., Bardelli, S., Bolzonella, M., Bongiorno, A., Cappi, A., Charlot, S., Ciliegi, P., Contini, T., Cucciati, O., de la Torre, S., Dolag, K., Foucaud, S., Franzetti, P., Gavignaud, I., Ilbert, O., Iovino, A., Lamareille, F., Marano, B., Mazure, A., Memeo, P., Merighi, R., Moscardini, L., Paltani, S., Pellò, R., Perez-Montero, E., Pozzetti, L., Radovich, M., Vergani, D., Zamorani, G., Zucca, E., 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 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), University of Oxford [Oxford], 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)-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 di Bologna, Dipartimento di Astronomia, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Guzzo L., Pierleoni M., Meneux B., Branchini E., Le Fevre O., Marinoni C., Garilli B., Blaizot J., De Lucia G., Pollo A., McCracken H.J., Bottini D., Le Brun V., Maccagni D., Picat J.-P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Bongiorno A., Cappi A., Charlot S., Ciliegi P., Contini T., Cucciati O., de La Torre S., Dolag K., Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Iovino A., Lamareille F., Marano B., Mazure A., Memeo P., Merighi R., Moscardini L., Paltani S., Pello' R., Perez-Montero E., Pozzetti L., Radovich M., Vergani D., Zamorani G., and Zucca E.
Subjects: High Energy Physics - Theory, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmological constant, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Cosmology, Metric expansion of space, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Redshift-space distortions, galaxies, 0103 physical sciences, 010303 astronomy & astrophysics, Physics, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], 010308 nuclear & particles physics, Astrophysics (astro-ph), Redshift survey, Redshift, Galaxy, High Energy Physics - Theory (hep-th), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Dark energy
Abstract: Observations of distant supernovae indicate that the Universe is now in a phase of accelerated expansion the physical cause of which is a mystery. Formally, this requires the inclusion of a term acting as a negative pressure in the equations of cosmic expansion, accounting for about 75 per cent of the total energy density in the Universe. The simplest option for this "dark energy" corresponds to a cosmological constant, perhaps related to the quantum vacuum energy. Physically viable alternatives invoke either the presence of a scalar field with an evolving equation of state, or extensions of general relativity involving higher-order curvature terms or extra dimensions. Although they produce similar expansion rates, different models predict measurable differences in the growth rate of large-scale structure with cosmic time. A fingerprint of this growth is provided by coherent galaxy motions, which introduce a radial anisotropy in the clustering pattern reconstructed by galaxy redshift surveys. Here we report a measurement of this effect at a redshift of 0.8. Using a new survey of more than 10,000 faint galaxies, we measure the anisotropy parameter b = 0.70 +/- 0.26, which corresponds to a growth rate of structure at that time of f = 0.91 +/- 0.36. This is consistent with the standard cosmological-constant model with low matter density and flat geometry, although the error bars are still too large to distinguish among alternative origins for the accelerated expansion. This could be achieved with a further factor-of-ten increase in the sampled volume at similar redshift., One PDF file including both main paper and Supplementary Information (28 pages, 3+2 figures). Published version available at http://www.nature.com/nature/journal/v451/n7178/abs/nature06555.html
Published: 2007

15. Coma cluster object populations down to M_R~-9.5

Author: Florence Durret, M. J. West, J. P. Picat, C. Adami, R. Pello, A. Mazure, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy, University of Hawaii, Services communs OMP (UMS 831), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-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), 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), 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: Absolute magnitude, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Coma (optics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Coma Cluster, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, education.field_of_study, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Space and Planetary Science, Globular cluster, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: This study follows a recent analysis of the galaxy luminosity functions and colour-magnitude red sequences in the Coma cluster (Adami et al. 2007). We analyze here the distribution of very faint galaxies and globular clusters in an east-west strip of $\sim 42 \times 7$ arcmin$^2$ crossing the Coma cluster center (hereafter the CS strip) down to the unprecedented faint absolute magnitude of M$_R \sim -9.5$. This work is based on deep images obtained at the CFHT with the CFH12K camera in the B, R, and I bands. The analysis shows that the observed properties strongly depend on the environment, and thus on the cluster history. When the CS is divided into four regions, the westernmost region appears poorly populated, while the regions around the brightest galaxies NGC 4874 and NGC 4889 (NGC 4874 and NGC 4889 being masked) are dominated by faint blue galaxies. They show a faint luminosity function slope of -2, very significantly different from the field estimates. Results are discussed in the framework of galaxy destruction (which can explain part of the very faint galaxy population) and of structures infalling on to Coma., To be published in A&A
Published: 2007
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16. The VIMOS VLT deep survey : the ultraviolet galaxy luminosity function and luminosity density at $3 \leq z \leq 4$

Author: Laurence Tresse, Daniela Vergani, A. Pollo, S. de la Torre, Paolo Ciliegi, P. Franzetti, E. Zucca, Olga Cucciati, Bruno Marano, A. Iovino, Sylvie Foucaud, A. Zanichelli, M. Scodeggio, S. Bardelli, M. Bondi, D. Bottini, Christian Marinoni, J. P. Picat, C. Adami, Lucia Pozzetti, O. Le Fevre, Luigi Guzzo, Olivier Ilbert, M. Radovich, Roberto Scaramella, A. Mazure, R. Merighi, Giampaolo Vettolani, S. Arnouts, Paola Merluzzi, Thierry Contini, V. Le Brun, Jarle Brinchmann, I. Gavignaud, G. Zamorani, Angela Bongiorno, C. J. Walcher, Bianca Garilli, B. Meneux, R. Pello, H. J. McCracken, F. Lamareille, S. Temporin, D. Maccagni, Stéphane Paltani, Yannick Mellier, A. Cappi, Micol Bolzonella, and Stephane Charlot
Subjects: Physics, education.field_of_study, statistics [galaxies], Star formation, Population, Extinction (astronomy), Astronomy and Astrophysics, Astrophysics, Galaxy, Luminosity, surveys, Space and Planetary Science, mass function, Magnitude (astronomy), Intergalactic travel, education, high-redshift [galaxies], Luminosity function (astronomy), luminosity function [galaxies]
Abstract: We study the LF of the high-z galaxy population with 3
Published: 2007

17. The SWIRE-VVDS-CFHTLS surveys: stellar mass assembly over the last 10 Gyears. Evidence for a major build up of the red sequence between z=2 and z=1

Author: A. Zanichelli, Sylvie Foucaud, D. Bottini, Stéphane Charlot, C. J. Walcher, J. P. Picat, P. Franzetti, A. Cappi, G. Vettolani, M. Polletta, M. Bolzonella, S. Temporin, Marco Scodeggio, D. Maccagni, O. Le Fevre, C. Adami, A. Pollo, Bruno Marano, Jason Surace, M. Radovich, T. Contini, H. J. McCracken, R. Pello, F. Lamareille, Luigi Guzzo, I. Gavignaud, Stephane Arnouts, S. Bardelli, A. Iovino, G. Zamorani, B. Meneux, Lucia Pozzetti, S. de la Torre, Paolo Ciliegi, E. Zucca, C. Lonsdale, V. Le Brun, O. Ilbert, S. Paltani, B. Garilli, D. Vergani, R. Merighi, C. Marinoni, R. Scaramella, Alain Mazure, L. Tresse, 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, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), 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), Services communs OMP (UMS 831), European Southern Observatory (ESO), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Arnouts S., Walcher C. J., Le Fèvre O., Zamorani G., Ilbert O., Le Brun V., Pozzetti L., Bardelli S., Tresse L., Zucca E., Charlot S., Lamareille F., McCracken H. J., Bolzonella M., Iovino A., Lonsdale C., Polletta M., Surace J., Bottini D., Garilli B., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Cappi A., Ciliegi P., Contini T., de La Torre S., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Radovich M., Temporin S., and Vergani D.
Subjects: GALAXIES: MASS FUNCTION, Active galactic nucleus, Stellar mass, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Global evolution, GALAXIES: LUMINOSITY FUNCTION, education, GALAXIES: FORMATION, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics
Abstract: (abridged abstract) We present an analysis of the stellar mass growth over the last 10 Gyrs using a large 3.6$\mu$ selected sample. We split our sample into active (blue) and quiescent (red) galaxies. Our measurements of the K-LFs and LD evolution support the idea that a large fraction of galaxies is already assembled at $z\sim 1.2$. Based on the analysis of the evolution of the stellar mass-to-light ratio (in K-band) for the spectroscopic sub-sample, we derive the stellar mass density for the entire sample. We find that the global evolution of the stellar mass density is well reproduced by the star formation rate derived from UV dust corrected measurements. Over the last 8Gyrs, we observe that the stellar mass density of the active population remains approximately constant while it gradually increases for the quiescent population over the same timescale. As a consequence, the growth of the stellar mass in the quiescent population must be due to the shutoff of star formation in active galaxies that migrate into the quiescent population. From $z=2$ to $z=1.2$, we observe a major build-up of the quiescent population with an increase by a factor of 10 in stellar mass, suggesting that we are observing the epoch when an increasing fraction of galaxies are ending their star formation activity and start to build up the red sequence., Comment: Accepted to A&A with major changes. 1 table and 13 figures
Published: 2007

18. The VIMOS-VLT Deep Survey. Galaxy luminosity function per morphological type up to z = 1.2

Author: Paolo Ciliegi, Angela Bongiorno, Paola Merluzzi, C. Adami, Marco Scodeggio, G. Mathez, Denis Burgarella, G. Busarello, Luigi Guzzo, Stéphane Charlot, D. Rizzo, S. Paltani, Roberto Scaramella, A. Zanichelli, H. J. McCracken, D. Maccagni, Lucia Pozzetti, M. Bolzonella, R. Merighi, O. Le Fevre, V. Le Brun, O. Ilbert, T. Contini, M. Bondi, D. Bottini, A. Cappi, Christian Marinoni, E. Zucca, S. Lauger, S. Arnout, R. Pello, G. Zamorani, L. Tresse, J. P. Picat, A. Pollo, Bruno Marano, P. Franzetti, I. Gavignaud, Mario Radovich, Sylvie Foucaud, A. Iovino, V. Ripepi, S. Bardelli, Yannick Mellier, G. Vettolani, V. Buat, B. Garilli, B. Meneux, M. Arnaboldi, Alain Mazure, 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), 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), 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), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, 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), 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Ilbert O., Lauger S., Tresse L., Buat V., Arnouts S., Le Fèvre 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., Merighi R., Paltani S., Pello R., Pollo A., Pozzetti L., Radovich M., Bondi M., Bongiorno A., Busarello G., Ciliegi P., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.
Subjects: GALAXIES: MASS FUNCTION, Population, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, Bulge, 0103 physical sciences, GALAXIES: EVOLUTION PARAMETERS, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, Galaxy: evolution, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Morphological type, Astronomy and Astrophysics, galaxies: fundamental parameters, Galaxy, Redshift, galaxies: luminosity function, Space and Planetary Science, mass function, Magnitude (astronomy), Elliptical galaxy
Abstract: Aims.We have computed the evolution of the rest-frame B-band luminosity function (LF) for bulge and disk-dominated galaxies since z=1.2. Methods: .We use a sample of 605 spectroscopic redshifts with IAB&leq; 24 in the Chandra Deep Field South from the VIMOS-VLT Deep Survey, 3555 galaxies with photometric redshifts from the COMBO-17 multi-color data, coupled with multi-color HST/ACS images from the Great Observatories Origin Deep Survey. We split the sample in bulge- and disk-dominated populations on the basis of asymmetry and concentration parameters measured in the rest-frame B-band. Results: .We find that at z=0.4-0.8, the LF slope is significantly steeper for the disk-dominated population (α=-1.19 ± 0.07) compared to the bulge-dominated population (α=-0.53 ± 0.13). The LF of the bulge-dominated population is composed of two distinct populations separated in rest-frame color: 68% of red (B-I)AB>0.9 and bright galaxies showing a strongly decreasing LF slope α=+0.55 ± 0.21, and 32% of blue (B-I)AB
Published: 2006
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19. Probing unexplored territories with MUSE: a second generation instrument for the VLT

Author: E. Popow, Antonio Manescau, Martin M. Roth, Harald Nicklas, Thierry Contini, Roser Pello, L. Capoani, Patrick Caillier, Remko Stuik, Didier Boudon, Christian Monstein, Stefan Dreizler, Luca Pasquini, Marijn Franx, Julien Devriendt, J. Gerssen, Herve Wozniak, Matthias Steinmetz, L. Parès, Aurélien Jarno, P. Ferruit, Richard M. McDermid, Eric Emsellem, Roland Bacon, P. T. de Zeeuw, Andreas Quirrenbach, Roland Reiss, T. Hahn, G. Soucail, Stefan Stroebele, P. Boehm, Peter M. Weilbacher, C. Petit, Bernard Delabre, M. Dupieux, Simon J. Lilly, C. M. Carollo, Florence Laurent, Johan Kosmalski, B. Guiderdoni, Jean-Louis Lizon, Svend M. Bauer, Eric Daguisé, Emmanuel Pecontal, Andreas Kelz, J.-P. Picat, S. Lynn, Joop Schaye, C. Koehler, Arlette Pécontal-Rousset, Wolfram Kollatschny, Edgard Renault, J. P. Dupin, D. Dalle, D. Hofmann, Jean-Pierre Dubois, G. Gallou, S. Brau-Nogué, Magali Loupias, and N. Champavert
Subjects: Physics, Supermassive black hole, Young stellar object, Milky Way, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Multi Unit Spectroscopic Explorer, Galaxy, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, Spectrograph, Astrophysics::Galaxy Astrophysics
Abstract: The Multi Unit Spectroscopic Explorer (MUSE) is a second-generation VLT panoramic integral-field spectrograph under preliminary design study. MUSE has a field of 1x1 arcmin**2 sampled at 0.2x0.2 arcsec**2 and is assisted by the VLT ground layer adaptive optics ESO facility using four laser guide stars. The simultaneous spectral range is 465-930 nm, at a resolution of R~3000. MUSE couples the discovery potential of a large imaging device to the measuring capabilities of a high-quality spectrograph, while taking advantage of the increased spatial resolution provided by adaptive optics. This makes MUSE a unique and tremendously powerful instrument for discovering and characterizing objects that lie beyond the reach of even the deepest imaging surveys. MUSE has also a high spatial resolution mode with 7.5x7.5 arcsec**2 field of view sampled at 25 milli-arcsec. In this mode MUSE should be able to obtain diffraction limited data-cubes in the 600-930 nm wavelength range. Although the MUSE design has been optimized for the study of galaxy formation and evolution, it has a wide range of possible applications; e.g. monitoring of outer planets atmosphere, environment of young stellar objects, super massive black holes and active nuclei in nearby galaxies or massive spectroscopic surveys of stellar fields in the Milky Way and nearby galaxies., Astronomical Telescopes and Instrumentation, SPIE 6265 Orlando 24-31May 2006 9 pages
Published: 2006

20. The VVDS: Early Results on the Large Scale Structure Distribution of Galaxies out to z~1.5

Author: I. Gavignaud, Marco Scodeggio, A. Zanichelli, G. Vettolani, C. Marinoni, Sylvie Foucaud, P. Franzetti, O. Le Fevre, A. Iovino, C. Adami, D. Rizzo, M. Arnaboldi, O. Ilbert, E. Zucca, Paolo Ciliegi, M. Bolzonella, Stephane Charlot, G. Busarello, R. Pello, D. Bottini, B. Garilli, D. Maccagni, A. Pollo, Stephane Arnouts, A. Cappi, B. Meneux, Lucia Pozzetti, S. Bardelli, T. Contini, L. Tresse, G. Mathez, Alain Mazure, R. Scaramella, S. Paltani, Paola Merluzzi, R. Merighi, G. Zamorani, M. Radovich, Bruno Marano, Luigi Guzzo, H. J. McCracken, J. P. Picat, Yannick Mellier, V. Le Brun, and M. Bondi
Subjects: Physics, Early results, Distribution (number theory), Scale structure, Astrophysics, Galaxy
Published: 2006
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21. The VIMOS VLT Deep Survey - Evolution of the luminosity functions by galaxy type up to z=1.5 from first epoch data

Author: G. Zamorani, Stéphane Charlot, J. P. Picat, O. Le Fevre, A. Cappi, S. Paltani, E. Zucca, D. Rizzo, O. Cucciati, D. Bottini, A. Pollo, Roberto Scaramella, R. Merighi, Stephane Arnouts, G. Busarello, Yannick Mellier, L. Gregorini, Lucia Pozzetti, Sylvie Foucaud, D. Maccagni, Paolo Ciliegi, M. Bolzonella, S. Bardelli, B. Garilli, V. Ripepi, Bruno Marano, M. Bondi, G. Vettolani, C. Adami, Magda Arnaboldi, T. Contini, H. J. McCracken, B. Meneux, F. Lamareille, R. Pello, Paola Merluzzi, Christian Marinoni, Mario Radovich, A. Iovino, G. Mathez, I. Gavignaud, Angela Bongiorno, Marco Scodeggio, P. Franzetti, L. Tresse, A. Zanichelli, Alain Mazure, V. Le Brun, O. Ilbert, Luigi Guzzo, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Bologna (OABO), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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), Istituto di Radioastronomia, Bologna, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), European Southern Observatory (ESO), INAF-Osservatorio Astronomico di Brera, 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), Zucca E., Ilbert O., Bardelli S., Tresse L., Zamorani G., Arnouts S., Pozzetti L., Bolzonella M., McCracken H. J., Bottini D., Garilli B., Le Brun V., Le Fevre O., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Cappi A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Iovino A., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pello' R., Pollo A., Radovich M., Bondi M., Bongiorno A., Busarello G., Cucciati O., Gregorini L., Lamareille F., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.
Subjects: Physics, 010308 nuclear & particles physics, Epoch (astronomy), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rest frame, Stellar classification, 01 natural sciences, Redshift, Galaxy, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Magnitude (astronomy), 10. No inequality, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract: From the first epoch observations of the VVDS up to z=1.5 we have derived luminosity functions (LF) of different spectral type galaxies. The VVDS data, covering ~70% of the life of the Universe, allow for the first time to study from the same sample and with good statistical accuracy the evolution of the LFs by galaxy type in several rest frame bands from a purely magnitude selected sample. The magnitude limit of the VVDS allows the determination of the faint end slope of the LF with unprecedented accuracy. Galaxies have been classified in four spectral classes, using their colours and redshift, and LFs have been derived in the U, B, V, R and I rest frame bands from z=0.05 to z=1.5. We find a significant steepening of the LF going from early to late types. The M* parameter is significantly fainter for late type galaxies and this difference increases in the redder bands. Within each of the galaxy spectral types we find a brightening of M* with increasing redshift, ranging from =< 0.5 mag for early type galaxies to ~1 mag for the latest type galaxies, while the slope of the LF of each spectral type is consistent with being constant with redshift. The LF of early type galaxies is consistent with passive evolution up to z~1.1, while the number of bright early type galaxies has decreased by ~40% from z~0.3 to z~1.1. We also find a strong evolution in the normalization of the LF of latest type galaxies, with an increase of more than a factor 2 from z~0.3 to z~1.3: the density of bright late type galaxies in the same redshift range increases of a factor ~6.6. These results indicate a strong type-dependent evolution and identifies the latest spectral types as responsible for most of the evolution of the UV-optical luminosity function out to z=1.5., 18 pages with encapsulated figures, revised version after referee's comments, accepted for publication in A&A
Published: 2006
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22. Deep and wide field imaging of the Coma cluster: the data

Author: C. Adami, J. P. Picat, C. Savine, A. Mazure, M. J. West, J. C. Cuillandre, R. Pelló, A. Biviano, C. J. Conselice, F. Durret, J. S. Gallagher, M. Gregg, C. Moreau, M. Ulmer, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire 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), Department of Physics and Astronomy, University of Hawaii, Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), INAF-Osservatorio Astronomico di Trieste (INAF-OATs), California Institute of Technology, Department of Astronomy (CALTECH), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), University of Wisconsin-Madison, Department of Physics, Le Conte Hall, University of California, Northwestern University, Evanston, and Beaussier, Catherine
Subjects: Physics, education.field_of_study, Astrophysics (astro-ph), Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrometry, Galaxy, Redshift, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cover (topology), [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, Magnitude (astronomy), Coma Cluster, education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Data reduction
Abstract: We have obtained deep and wide field imaging of the Coma cluster of galaxies with the CFH12K camera at CFHT in the B, V, R and I filters. In this paper, we present the observations, data reduction, catalogs and first scientific results. We investigated the quality of our data by internal and external literature comparisons. We also checked the realisation of the observational requirements we set. Our observations cover two partially overlapping areas of $42 \times 28$ arcmin$^2$, leading to a total area of 0.72 $\times$ 0.82 deg$^2$. We have produced catalogs of objects that cover a range of more than 10 magnitudes and are complete at the 90% level at B$\sim$25, V$\sim$24, R$\sim$24 and I$\sim$23.5 for stellar-like objects, and at B$\sim$22, V$\sim$21, R$\sim$20.75 and I$\sim$20.5 for faint low-surface-brightness galaxy-like objects. Magnitudes are in good agreement with published values from R$\sim$16 to R$\sim$25. The photometric uncertainties are of the order of 0.1 magnitude at R$\sim$20 and of 0.3 magnitude at R$\sim$25. Astrometry is accurate to 0.5~arcsec and also in good agreement with published data. Our catalog provides a rich dataset that can be mined for years to come to gain new insights into the formation and evolution of the Coma cluster and its galaxy population. As an illustration of the data quality, we examine the bright part of the Colour Magnitude Relation (B-R versus R) derived from the catalog and find that it is in excellent agreement with that derived for galaxies with redshifts in the Coma cluster, and with previous CMRs estimated in the literature., A&A, 2006, 451, 1159. Catalog available at http://cencosw.oamp.fr/ with no restriction. High resolution figures can be found at A&A, 2006, 451, 1159
Published: 2006
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23. The VIMOS VLT Deep Survey: the build-up of the colour-density relation

Author: V. Le Brun, O. Ilbert, C. Adami, G. Zamorani, G. Busarello, Marco Scodeggio, Gianpaolo Vettolani, H. J. McCracken, D. Maccagni, Paola Merluzzi, Stéphane Paltani, I. Gavignaud, E. Zucca, D. Rizzo, B. Garilli, M. Bolzonella, Christian Marinoni, Angela Bongiorno, A. Cappi, Luigi Guzzo, T. Contini, D. Vergani, R. Pello, L. Gregorini, G. Mathez, L. Tresse, Magda Arnaboldi, Mario Radovich, F. Lamareille, Stéphane Charlot, G. Temporin, A. Pollo, S. Bardelli, Stephane Arnouts, A. Zanichelli, Lucia Pozzetti, Paolo Ciliegi, V. Ripepi, Yannick Mellier, Alain Mazure, D. Bottini, O. Le Fevre, P. Franzetti, M. Bondi, J. P. Picat, Sylvie Foucaud, O. Cucciati, S. de la Torre, Bruno Marano, Roberto Scaramella, A. Iovino, R. Merighi, B. Meneux, INAF-Osservatorio Astronomico di Brera, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Bologna (OABO), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), IRA-INAF, Bologna, 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-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), European Southern Observatory (ESO), INTEGRAL Science Data Centre, 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: Physics, 010504 meteorology & atmospheric sciences, Star formation, Diagram, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Function (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rest frame, 01 natural sciences, Redshift, Bin, Galaxy, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
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), depth (I_AB, 17 pages, 10 figures, figures added, accepted by A&A
Published: 2006
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24. Spatial variations of the optical galaxy luminosity functions and red sequences in the Coma cluster: clues to its assembly history

Author: R. Pello, C. Adami, J. P. Picat, B. Meneux, Florence Durret, M. J. West, A. Mazure, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (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, Department of Physics and Astronomy, University of Hawaii, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), and Beaussier, Catherine
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Coma (optics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Coma Cluster, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Late type, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Early type, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Magnitude (astronomy), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Clusters of galaxies are believed to be at the intersections of cosmological filaments and to grow by accreting matter from these filaments. Such continuous infall has major consequences not only on clusters but also on the physics of cluster galaxies. Faint galaxies are particularly interesting as they are very sensitive to environmental effects, and may have a different behaviour from that of bright galaxies. The aim of this paper is to sample the Coma cluster building history, based on the analysis of galaxy luminosity functions and red sequences in the Color Magnitude Relation down to faint magnitudes, which are privileged tools for this purpose. The present analysis is based on deep (R~24), wide (~0.5 deg2) multiband (BVRI Vega system) images of the Coma cluster obtained with the CFH12K camera at the CFHT. We have derived LFs and CMRs in twenty 10x10 arcmin2 regions and in larger regions. In all photometric bands, we found steeply rising LFs in the north-northeast half of the cluster (due to early type galaxies at bright magnitudes and due to late type galaxies at the faint end), and much flatter LFs in the south-southwest region. Although the fine behaviour of the CMR RS is different in these two regions, a good agreement is found in general between the RS computed for faint and for bright galaxies. All these results can be interpreted consistently in the framework of the building up process previously proposed. The Northern Coma area is a relatively quiescent region while the southern area experiences several infalls., Comment: To be published in A&A, several figures in jpg format, full resolution figures and paper available at http://cencosw.oamp.fr/ under the Coma page. The lacking figures are available at the same adress. Updated CFHT acknowledgements and aa format
Published: 2006
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25. The VIMOS-VLT Deep Survey. The evolution of galaxy clustering per spectral type to z ~= 1.5

Author: Christian Marinoni, T. Contini, Luigi Guzzo, Paolo Ciliegi, G. Zamorani, A. Cappi, O. Cucciati, Angela Bongiorno, L. Tresse, Stephane Arnouts, Lucia Pozzetti, Yannick Mellier, V. Ripepi, E. Zucca, D. Rizzo, V. LeBrun, S. Paltani, Roberto Scaramella, Stéphane Charlot, G. Mathez, O. LeFevre, R. Merighi, I. Gavignaud, A. Zanichelli, M. Bondi, B. Meneux, D. Bottini, Alain Mazure, G. Vettolani, J. P. Picat, M. Bolzonella, A. Iovino, R. Pello, M. Arnaboldi, G. Busarello, B. Garilli, Marco Scodeggio, C. Adami, L. Gregorini, Mario Radovich, F. Lamareille, P. Franzetti, Paola Merluzzi, O. Ilbert, Bruno Marano, D. Maccagni, H. J. McCracken, Sylvie Foucaud, A. Pollo, S. Bardelli, 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 (INAF-OAB), INAF-Osservatorio Astronomico di Bologna (OABO), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), INAF-Osservatorio Astronomico di Brera, 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), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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-Osservatorio Astronomico di Roma (INAF-OAR), IRA-INAF, Bologna, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), School of Physics and Astronomy, University of Nottingham, European Southern Observatory (ESO), INTEGRAL Science Data Centre, 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), Meneux B., Le Fèvre O., Guzzo L., Pollo A., Cappi A., Ilbert O., Iovino A., Marinoni C., McCracken H. J., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Arnaboldi M., Bardelli S., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P., Gavignaud I., Marano B., Mazure A., Merighi R., Paltani S., Pello' R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Cucciati O., Gregorini L., Lamareille F., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.
Subjects: Population, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Type (model theory), Stellar classification, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 10. No inequality, education, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Space and Planetary Science, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We measure the evolution of clustering for galaxies with different spectral types from 6495 galaxies with 17.51.2, due to the growth in clustering of the star-forming population. We find similar results when splitting the sample into `red' and `blue' galaxies using the observed color bi-modality. When compared to the expected linear growth of mass fluctuations, a natural interpretation of these observations is that: (a) the assembly of massive early type galaxies is already mostly complete in the densest dark matter halos at z~=1; (b) luminous late-type galaxies are located in higher-density, more clustered regions of the Universe at z~=1.5 than at present, indicating that star formation activity is progressively increasing, going back in time, in the higher-density peaks that today are mostly dominated by old galaxies., 12 pages, Accepted on 11-Feb-06 for publication in Astronomy and Astrophysics
Published: 2006
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26. Accurate photometric redshifts for the CFHT Legacy Survey calibrated using the VIMOS VLT Deep Survey

Author: Paolo Ciliegi, G. Busarello, R. Pello, Mario Radovich, A. Pollo, V. Ripepi, A. Iovino, V. Le Brun, O. Ilbert, T. Contini, C. Adami, L. Tresse, S. Bardelli, M. Bondi, Christian Marinoni, O. Le Fevre, D. Vergani, I. Gavignaud, Marco Scodeggio, B. Garilli, D. Maccagni, E. Zucca, D. Rizzo, Stéphane Paltani, Gianpaolo Vettolani, H. J. McCracken, P. Franzetti, Bruno Marano, Alain Mazure, M. Bolzonella, Yannick Mellier, Sylvie Foucaud, Roberto Scaramella, R. Merighi, D. Bottini, A. Cappi, Luigi Guzzo, O. Cucciati, S. de la Torre, L. Gregorini, J. P. Picat, E. Bertin, B. Meneux, G. Mathez, Paola Merluzzi, Angela Bongiorno, Stéphane Charlot, Stephane Arnouts, Lucia Pozzetti, G. Zamorani, F. Lamareille, A. Zanichelli, 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), Ilbert O., Arnouts S., McCracken H. J., Bolzonella M., Bertin E., Le Fèvre O., Mellier Y., Zamorani G., Pellò R., Iovino A., Tresse L., Le Brun V., Bottini D., Garilli B., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Bardelli S., Cappi A., Charlot S., Ciliegi P., Contini T., Cucciati O., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pollo A., Pozzetti L., Radovich M., Zucca E., Bondi M., Bongiorno A., Busarello G., de La Torre S., Gregorini L., Lamareille F., Mathez G., Merluzzi P., Ripepi V., Rizzo D., Vergani D., Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Bologna (OABO), 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-Osservatorio Astronomico di Brera, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), INAF-Osservatorio Astronomico di Roma (INAF-OAR), IRA-INAF, Bologna, School of Physics and Astronomy, University of Nottingham, European Southern Observatory (ESO), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), INTEGRAL Science Data Centre, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), 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: FOS: Physical sciences, METHODS: DATA ANALYSIS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Extended Groth Strip, 0103 physical sciences, Calibration, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Sigma, Astronomy and Astrophysics, GALAXIES: PHOTOMETRY, Cosmic variance, Galaxy, Redshift, Cover (topology), 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], GALAXIES: DISTANCES AND REDSHIFTS
Abstract: We present photometric redshifts for an uniquely large and deep sample of 522286 objects with i'_{AB}, Comment: 19 pages, 17 figures, submitted to A&A. The photometric redshifts described in this paper will be made publicly available from 1st may 2006 at http://terapix.iap.fr and http://cencosw.oamp.fr/
Published: 2006
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27. The VIMOS-VLT Deep Survey: Luminosity dependence of clustering at z~1

Author: A. Pollo, L. Guzzo, O. Le Fèvre, B. Meneux, A. Cappi, P. Franzetti, A. Iovino, H. J. McCracken, C. Marinoni, G. Zamorani, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, I. Gavignaud, O. Ilbert, B. Marano, A. Mazure, R. Merighi, S. Paltani, R. Pellò, L. Pozzetti, M. Radovich, E. Zucca, M. Bondi, A. Bongiorno, G. Busarello, O. Cucciati, L. Gregorini, F. Lamareille, G. Mathez, Y. Mellier, P. Merluzzi, V. Ripepi, D. Rizzo, 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), Pollo A., Guzzo L., Le Fèvre O., Meneux B., Cappi A., Franzetti P., Iovino A., McCracken H. J., Marinoni C., Zamorani G., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Charlot S., Ciliegi P., Contini T., Foucaud S., Gavignaud I., Ilbert O., Marano B., Mazure A., Merighi R., Paltani S., Pello R., Pozzetti L., Radovich M., Zucca E., Bondi M., Bongiorno A., Busarello G., Cucciati P., Gregorini L., Lamareille F., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.
Subjects: Absolute magnitude, statistical [methods], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], large scale structure of Universe [cosmology], 0103 physical sciences, Cluster analysis, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Redshift, observations [cosmology], Correlation function (statistical mechanics), Space and Planetary Science, Halo, VIMOS-VLT Deep Survey
Abstract: We investigate the dependence of galaxy clustering on the galaxy intrinsic luminosity at high redshift, using the data from the First Epoch VIMOS-VLT Deep Survey (VVDS). The size (6530 galaxies) and depth (I_{AB}=0.9 and median absolute magnitude -19.6< M_B < -21.3. Fitting w_p(r_p) with a single power-law model for the real-space correlation function xi(r)=(r/r_0)^{-gamma}, we measure the relationship of the correlation length r_0 and the slope gamma with the sample median luminosity for the first time at such high redshift. Values from our lower-redshift samples (0.1=-19.6) have a correlation length r_0=2.7^{+0.3}_{-0.3} h^{-1} Mpc, compared to r_0=5.0^{+1.5}_{-1.6} h^{-1} Mpc at =-21.3. Correspondingly the slope of the correlation function is observed to steepen significantly from \gamma=1.6^{+0.1}_{-0.1} to \gamma=2.4^{+0.4}_{-0.2}. This is not observed neither by large local surveys nor in our lower-redshift sample and seems to imply a significant change in the way luminous galaxies trace dark-matter halos at z~1 with respect to z~0. At our effective median redshift z~0.9 this corresponds to a strong difference of the relative bias, from b/b* < 0.7 for galaxies with L < L*, to b/b*~1.4 for galaxies with L > L*., Comment: Accepted for publication in Astronomy and Astrophysics
Published: 2006
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28. A large population of galaxies 9 to 12 billion years back in the history of the Universe

Author: D. Rizzo, C. Adami, M. Bolzonella, Marco Scodeggio, Roberto Scaramella, A. Mazure, Lucia Pozzetti, A. Zanichelli, Paola Merluzzi, E. Zucca, B. Meneux, R. Merighi, Thierry Contini, O. Ilbert, G. Busarello, Christian Marinoni, V. Le Brun, Sylvie Foucaud, I. Gavignaud, G. Vettolani, G. Mathez, V. Ripepi, J. P. Picat, B. Garilli, R. Pello, D. Maccagni, Stephane Charlot, Mario Radovich, G. Zamorani, Stéphane Paltani, Yannick Mellier, M. Arnaboldi, Bruno Marano, A. Iovino, F. Lamareille, A. Cappi, M. Bondi, Luigi Guzzo, Laurence Tresse, A. Pollo, S. Bardelli, D. Bottini, Stéphane Arnouts, Angela Bongiorno, H. J. McCracken, L. Gregorini, P. Franzetti, O. Le Fevre, Paolo Ciliegi, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), 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 Astrophysik (MPA), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Le Fèvre O., Paltani S., Arnouts S., Charlot S., Foucaud S., Ilbert O., McCracken H. J., Zamorani G., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Bardelli S., Bolzonella M., Cappi A., Ciliegi P., Contini T., Franzetti P., Gavignaud I., Guzzo L., Iovino A., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Pellò R., Pollo A., Pozzetti L., Radovich M., Zucca E., Arnaboldi M., Bondi, M., Bongiorno A., Busarello G., Gregorini L., Lamareille F., Mathez G., Mellier, Y., Merluzzi P., Ripepi V., Rizzo D., 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 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: 010504 meteorology & atmospheric sciences, Radio galaxy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Peculiar galaxy, GALASSIE, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Luminous infrared galaxy, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), Astronomy, Quasar, COSMOLOGIA, Galaxy, Elliptical galaxy
Abstract: To understand the evolution of galaxies, we need to know as accurately as possible how many galaxies were present in the Universe at different epochs. Galaxies in the young Universe have hitherto mainly been identified using their expected optical colours, but this leaves open the possibility that a significant population remains undetected because their colours are the result of a complex mix of stars, gas, dust or active galactic nuclei. Here we report the results of a flux-limited I-band survey of galaxies at look-back times of 9 to 12 billion years. We find 970 galaxies with spectroscopic redshifts between 1.4 and 5. This population is 1.6 to 6.2 times larger than previous estimates, with the difference increasing towards brighter magnitudes. Strong ultraviolet continua (in the rest frame of the galaxies) indicate vigorous star formation rates of more than 10 to 100 solar masses per year. As a consequence, the cosmic star formation rate is higher than previously measured at redshifts of 3 to 4., Comment: Published in Nature, 22 September 2005
Published: 2005
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29. The Vimos-VLT Deep Survey: Results from the First-Epoch Observations

Author: R. Pello, Mario Radovich, B. Meneux, Paolo Ciliegi, Vincenzo Ripepi, Stephane Charlot, H. J. McCracken, M. Bondi, Alain Mazure, C. Adami, G. Busarello, E. Zucca, Marco Scodeggio, D. Rizzo, D. Bottini, V. Le Brun, Bruno Marano, B. Garilli, I. Gavignaud, D. Maccagni, O. Ilbert, Yannick Mellier, C. Marinoni, S. Paltani, Roberto Scaramella, L. Tresse, R. Merighi, Sylvie Foucaud, A. Pollo, T. Contini, L. Gregorini, M. Bolzonella, Paola Merluzzi, Angela Bongiorno, G. Vettolani, Luigi Guzzo, P. Franzetti, G. Mathez, Magda Arnaboldi, A. Cappi, S. Bardelli, O. Le Fevre, J. P. Picat, A. Iovino, G. Zamorani, Stephane Arnouts, Lucia Pozzetti, A. Zanichelli, 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), Yannick Mellier, Georges Meylan, YANNICK MELLIER AND GEORGES MEYLAN, Paltani S., Ilbert O., Le Fèvre O., Marinoni C., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.-P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Contini T., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Iovino A., McCracken H. J., Marano B., Mazure A., Meneux B., Merighi R., Pellò R., Pollo A., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Ciliegi P., Gregorini L., Mathez G., Mellier Y., Merluzzi P., Ripepi V., Rizzo D, 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: Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, Astronomy and Astrophysics, Function (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift survey, Galaxy, Redshift, Spectral line, Luminosity, Space and Planetary Science, Limiting magnitude, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract: ISBN 0521851963; The Vimos-VLT Deep Survey is a spectroscopic survey aiming at collecting more than 50000 spectra down to a limiting magnitude IAB=24, and 100000 down to IAB=22.5, on a total of about 16 deg2 without any color or morphology preselection. We present the N(z) distribution up to z~ 5, obtained from a purely magnitude-limited sample down to IAB=24, which is an important input to weak-lensing studies. We discuss the evolution of the galaxy luminosity function up to z~ 2, which exhibits a very strong increase in the typical galaxy luminosity Delta M*&simeq; -2.5 in the U band compared to the local value. Surveys like the VVDS also allow to study the galaxy bias as a function of redshift without assumption about its linearity, an assumption that we find to be violated in some cases. A low bias is found, and the linear bias is shown to increase with redshift.
Published: 2005
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30. The VIRMOS deep imaging survey IV: Near-infrared observations

Author: Thierry Contini, I. Gavignaud, G. Zamorani, M. Scodeggio, O. Le Fevre, M. Radovich, G. Mathez, Bianca Garilli, G. Busarello, H. J. McCracken, Stéphane Arnouts, Giampaolo Vettolani, D. Maccagni, Paola Merluzzi, Stéphane Paltani, Stephane Charlot, D. Bottini, L. Gregorini, Paolo Saracco, R. Pello, Bruno Marano, A. Zanichelli, Yannick Mellier, A. Cappi, Emmanuel Bertin, Olivier Ilbert, B. Meneux, A. Iovino, Paolo Ciliegi, Olga Cucciati, A. Pollo, Roberto Scaramella, A. Mazure, Lucia Pozzetti, R. Merighi, S. Bardelli, J. P. Picat, Magda Arnaboldi, Laurence Tresse, M. Bondi, E. Zucca, D. Rizzo, L. Paioro, V. Le Brun, P. Franzetti, Luigi Guzzo, Angela Bongiorno, Vincenzo Ripepi, Sylvie Foucaud, Christian Marinoni, M. Bolzonella, C. Adami, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), 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), Services communs OMP (UMS 831), 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 - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Capodimonte (OAC), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, European Southern Observatory (ESO), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Departement de Radioastronomie Millimétrique (DEMIRM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), 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), Università di Bologna, Dipartimento di Astronomia, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), École normale supérieure - Paris (ENS Paris), Iovino A., McCracken H. J., Garilli B., Foucaud S., Le Fèvre O., Maccagni D., Saracco P., Bardelli S., Busarello G., Scodeggio M., Zanichelli A., Paioro L., Bottini D., Le Brun V., Picat J. P., Scaramella R., Tresse L., Vettolani G., Adami C., Arnaboldi M., Arnouts S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T., Franzetti P., Gavignaud I., Guzzo L., Ilbert O., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo A., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bertin E., Bondi M., Bongiorno A., Cucciati O., Gregorini L., Mathez G., Mellier Y., Merluzzi P., Ripepi V., and Rizzo D.
Subjects: FOS: Physical sciences, Magnitude (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, GALAXIES: SURVEYS, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, 0103 physical sciences, Cluster analysis, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Near-infrared spectroscopy, Astronomy and Astrophysics, galaxies: general, cosmology: large-scale structure of Universe, Galaxy, Wavelength, Amplitude, 13. Climate action, Space and Planetary Science, Limiting magnitude
Abstract: In this paper we present a new deep, wide-field near-infrared imaging survey. Our J- and K-band observations in four separate fields complement optical BVRI, ultraviolet and spectroscopic observations undertaken as part of the VIMOS-VLT deep survey (VVDS). In total, our survey spans ~400arcmis^2. Our catalogues are reliable in all fields to at least Kvega~20.75 and Jvega~21.50 (defined as the magnitude where object contamination is less than 10% and completeness greater than 90%). Taken together these four fields represents a unique combination of depth, wavelength coverage and area. We describe the complete data reduction process and outline a comprehensive series of tests carried out to characterise the reliability of the final catalogues. We compare the statistical properties of our catalogues with literature compilations. We find that our J- and K-selected galaxy counts are in good agreement with previously published works, as are our (J-K) versus K colour-magnitude diagrams. Stellar number counts extracted from our fields are consistent with a synthetic model of our galaxy. Using the location of the stellar locus in colour-magnitude space and the measured field-to-field variation in galaxy number counts we demonstrate that the absolute accuracy of our photometric calibration is at the 5% level or better. Finally, an investigation of the angular clustering of K- selected extended sources in our survey displays the expected scaling behaviour with limiting magnitude, with amplitudes in each magnitude bin in broad agreement with literature values., 15 pages, 19 figs, Accepted by A&A
Published: 2005
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31. The VIMOS VLT deep survey. Computing the two point correlation statistics and associated uncertainties

Author: A. Pollo, B. Meneux, L. Guzzo, O. Le Fèvre, J. Blaizot, A. Cappi, A. Iovino, C. Marinoni, H. J. McCracken, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, M. Arnaboldi, S. Arnouts, S. Bardelli, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, O. Ilbert, B. Marano, G. Mathez, A. Mazure, R. Merighi, S. Paltani, R. Pellò, L. Pozzetti, M. Radovich, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, G. Busarello, L. Gregorini, F. Lamareille, Y. Mellier, P. Merluzzi, V. Ripepi, D. Rizzo, INAF-Osservatorio Astronomico di Brera (INAF-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), INAF-Osservatorio Astronomico di Bologna (OABO), INAF-Osservatorio Astronomico di Brera, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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-Osservatorio Astronomico di Roma (INAF-OAR), Istituto di Radioastronomia, Bologna, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Max-Planck-Institut für Astrophysik (MPA), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Pollo A., Meneux B., Guzzo L., Le Fèvre O., Blaizot J., Cappi A., Iovino A., Marinoni C., McCracken H. J., Bottini D., Garilli B., Le Brun V., Maccagni D., Picat J.P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., 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., Pello R., Pozzetti L., Radovich M., Zamorani G., Zucca E., Bondi M., Bongiorno A., Busarello G., Gregorini L., Lamareille F., Mellier Y., Merluzzi P., Ripepi V., Rizzo D., 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: Physics, COSMIC cancer database, 010308 nuclear & particles physics, Epoch (reference date), Astrophysics (astro-ph), FOS: Physical sciences, Sampling (statistics), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Correlation function (statistical mechanics), Space and Planetary Science, 0103 physical sciences, Statistics, Galaxy formation and evolution, Cluster analysis, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, VIMOS-VLT Deep Survey
Abstract: We are presenting in this paper a detailed account of the methods used to compute the three-dimensional two-point galaxy correlation function in the VIMOS-VLT deep survey (VVDS). We investigate how instrumental selection effects and observational biases affect the measurements and identify the methods to correct them. We quantify the accuracy of our correction method using an ensemble of fifty mock galaxy surveys generated with the GalICS semi-analytic model of galaxy formation which incorporate the same selection biases and tiling strategy as the real data does. We demonstrate that we are able to recover the real-space two-point correlation function xi(s) to an accuracy better than 10% on scales larger than 1 h^{-1} Mpc, and of about 30% on scales below 1 h^{-1} Mpc, with the sampling strategy used for the first epoch VVDS data. The projected correlation function w_p(r_p) is recovered with an accuracy better than 10% on all scales 0.1, 16 pages, accepted 10-Mar-05 in A&A
Published: 2005
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32. The GALEX VIMOS-VLT Deep Survey Measurement of the Evolution of the 1500 Å Luminosity Function

Author: S. Arnouts, D. Schiminovich, O. Ilbert, L. Tresse, B. Milliard, M. Treyer, S. Bardelli, T. Budavari, T. K. Wyder, E. Zucca, O. Le Fèvre, D. C. Martin, G. Vettolani, C. Adami, M. Arnaboldi, T. Barlow, L. Bianchi, M. Bolzonella, D. Bottini, Y.-I. Byun, A. Cappi, S. Charlot, T. Contini, J. Donas, K. Forster, S. Foucaud, P. Franzetti, P. G. Friedman, B. Garilli, I. Gavignaud, L. Guzzo, T. M. Heckman, C. Hoopes, A. Iovino, P. Jelinsky, V. Le Brun, Y.-W. Lee, D. Maccagni, B. F. Madore, R. Malina, B. Marano, C. Marinoni, H. J. McCracken, A. Mazure, B. Meneux, R. Merighi, P. Morrissey, S. Neff, S. Paltani, R. Pellò, J. P. Picat, A. Pollo, L. Pozzetti, M. Radovich, R. M. Rich, R. Scaramella, M. Scodeggio, M. Seibert, O. Siegmund, T. Small, A. S. Szalay, B. Welsh, C. K. Xu, G. Zamorani, A. Zanichelli, 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), Schiminovich D., Ilbert O., Arnouts S., Milliard B., Tresse L., Le Fèvre O., Treyer M., Wyder T. K., Budavári T., Zucca E., Zamorani G., Martin D. C., Adami C., Arnaboldi M., Bardelli S., Barlow T., Bianchi L., Bolzonella M., Bottini D., Byun Y.I., Cappi A., Contini T., Charlot S., Donas J., Forster K., Foucaud S., Franzetti P., Friedman P. G., Garilli B., Gavignaud I., Guzzo L., Heckman T. M., Hoopes C., Iovino A., Jelinsky P., Le Brun V., Lee Y.W., Maccagni D., Madore B. F., Malina R., Marano B., Marinoni C., McCracken H. J., Mazure A., Meneux B., Morrissey P., Neff S., Paltani S., Pellò R., Picat J. P., Pollo A., Pozzetti L., Radovich M., Rich R. M., Scaramella R., Scodeggio M., Seibert M., Siegmund O., Small T., Szalay A. S., Vettolani G., Welsh B., Xu C. K., Zanichelli A., 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: Physics, GALAXIES: MASS FUNCTION, Number density, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, media_common.quotation_subject, Galaxies: Luminosity Function, Astronomy and Astrophysics, Astrophysics, Ultraviolet: Galaxies, 01 natural sciences, Cosmology: Observations, Redshift, Universe, Galaxy, Luminosity, Mass Function, Space and Planetary Science, 0103 physical sciences, Galaxies: Evolution, 010303 astronomy & astrophysics, Luminosity function (astronomy), media_common
Abstract: We present the first measurement of the galaxy luminosity function (LF) at 1500 Å in the range 0.2=alpha>=-1.65, with a marginally significant hint of increase at higher z. (3) We split the sample in three rest-frame (B-I) intervals, providing an approximate spectral type classification: Sb-Sd, Sd-Irr, and unobscured starbursts. We find that the bluest class evolves less strongly in luminosity than the two other classes. On the other hand, their number density increases sharply with z (~15% in the local universe to ~55% at z~1), while that of the reddest classes decreases.
Published: 2005
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33. The GALEX-VVDS Measurement of the Evolution of the Far-Ultraviolet Luminosity Density and the Cosmic Star Formation Rate

Author: D. Schiminovich, O. Ilbert, S. Arnouts, B. Milliard, L. Tresse, O. Le Fèvre, M. Treyer, T. K. Wyder, T. Budavári, E. Zucca, G. Zamorani, D. C. Martin, C. Adami, M. Arnaboldi, S. Bardelli, T. Barlow, L. Bianchi, M. Bolzonella, D. Bottini, Y.-I. Byun, A. Cappi, T. Contini, S. Charlot, J. Donas, K. Forster, S. Foucaud, P. Franzetti, P. G. Friedman, B. Garilli, I. Gavignaud, L. Guzzo, T. M. Heckman, C. Hoopes, A. Iovino, P. Jelinsky, V. Le Brun, Y.-W. Lee, D. Maccagni, B. F. Madore, R. Malina, B. Marano, C. Marinoni, H. J. McCracken, A. Mazure, B. Meneux, P. Morrissey, S. Neff, S. Paltani, R. Pellò, J. P. Picat, A. Pollo, L. Pozzetti, M. Radovich, R. M. Rich, R. Scaramella, M. Scodeggio, M. Seibert, O. Siegmund, T. Small, A. S. Szalay, G. Vettolani, B. Welsh, C. K. Xu, A. Zanichelli, 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), Schiminovich D., Ilbert O., Arnouts S., Milliard B., Tresse L., Le Fèvre O., Treyer M., Wyder T. K., Budavári T., Zucca E., Zamorani G., Martin D. C., Adami C., Arnaboldi M., Bardelli S., Barlow T., Bianchi L., Bolzonella M., Bottini D., Byun Y.I., Cappi A., Contini T., Charlot S., Donas J., Forster K., Foucaud S., Franzetti P., Friedman P. G., Garilli B., Gavignaud I., Guzzo L., Heckman T. M., Hoopes C., Iovino A., Jelinsky P., Le Brun V., Lee Y.W., Maccagni D., Madore B. F., Malina R., Marano B., Marinoni C., McCracken H. J., Mazure A., Meneux B., Morrissey P., Neff S., Paltani S., Pellò R., Picat J. P., Pollo A., Pozzetti L., Radovich M., Rich R. M., Scaramella R., Scodeggio M., Seibert M., Siegmund O., Small T., Szalay A. S., Vettolani G., Welsh B., Xu C. K., Zanichelli A., 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: GALAXIES: MASS FUNCTION, Galaxies: Luminosity Function, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Ultraviolet: Galaxies, medicine.disease_cause, 01 natural sciences, Cosmology: Observations, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxies: Evolution, medicine, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, COSMIC cancer database, 010308 nuclear & particles physics, Star formation, Attenuation, Astrophysics (astro-ph), Astronomy and Astrophysics, Redshift, Galaxy, Mass Function, Space and Planetary Science, Ultraviolet
Abstract: In a companion paper (Arnouts et al. 2004) we presented new measurements of the galaxy luminosity function at 1500 Angstroms out to z~1 using GALEX-VVDS observations (1039 galaxies with NUV0.2) and at higher z using existing data sets. In this paper we use the same sample to study evolution of the FUV luminosity density. We detect evolution consistent with a (1+z)^{2.5+/-0.7} rise to z~1 and (1+z)^{0.5+/-0.4} for z>1. The luminosity density from the most UV-luminous galaxies (UVLG) is undergoing dramatic evolution (x30) between 025%) of the total FUV luminosity density at z, Comment: This paper will be published as part of the Galaxy Evolution Explorer (GALEX) Astrophysical Journal Letters Special Issue. Links to the full set of papers will be available at http://www.galex.caltech.edu/PUBLICATIONS/ after November 22, 2004
Published: 2005
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34. The Vimos VLT Deep Survey: Compact structures in the CDFS

Author: C. Adami, A. Mazure, O. Ilbert, A. Cappi, D. Bottini, B. Garilli, V. Le Brun, O. Le Fèvre, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, M. Arnaboldi, S. Arnouts, S. Bardelli, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, G. Covone, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, A. Iovino, S. Lauger, H. J. McCracken, B. Marano, C. Marinoni, B. Meneux, R. Merighi, S. Paltani, R. Pellò, A. Pollo, L. Pozzetti, M. Radovich, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, G. Busarello, L. Gregorini, G. Mathez, Y. Mellier, P. Merluzzi, V. Ripepi, D. Rizzo, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Bologna (OABO), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), 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), IRA-INAF, Bologna, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Astrophysik (MPA), 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), European Southern Observatory (ESO), INAF-Osservatorio Astronomico di Brera, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), 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), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Beaussier, Catherine, Adami, C., Mazure, A., Ilbert, O., Cappi, A., Bottini, D., Garilli, B., Le Brun, V., Le Fèvre, O., Maccagni, D., Picat, J. P., Covone, Giovanni, Franzetti, P., Gavignaud, I., and VVSD Consortium
Subjects: Physics, education.field_of_study, Lower velocity, Population, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Redshift, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Chandra Deep Field South, Low Mass, education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], VIMOS-VLT Deep Survey, Astrophysics::Galaxy Astrophysics, Photometric redshift
Abstract: We have used the Vimos VLT Deep Survey in combination with other spectroscopic, photometric and X-ray surveys from literature to detect several galaxy structures in the Chandra Deep Field South (CDFS). Both a friend-of-friend based algorithm applied to the spectroscopic redshift catalog and an adaptative kernel galaxy density and colour maps correlated with photometric redshift estimates have been used. We mainly detect a chain-like structure at z=0.66 and two massive groups at z=0.735 and 1.098 showing signs of ongoing collapse. We also detect two galaxy walls at z=0.66 and at z=0.735 (extremely compact in redshift space). The first one contains the chain-like structure and the last one contains in its center one of the two massive groups. Finally, other galaxy structures that are probably loose low mass groups are detected. We compare the group galaxy population with simulations in order to assess the richness of these structures and we study their galaxy morphological contents. The higher redshift structures appear to probably have lower velocity dispersion than the nearby ones. The number of moderatly massive structures we detect is consistent with what is expected for an LCDM model, but a larger sample is required to put significant cosmological constraints., Comment: 15 pages, 17 figures, accepted in A&A
Published: 2005
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35. The VVDS-VLA deep field. II. Optical and near infrared identifications of VLA S1.4 GHz > 80 mu Jy sources in the VIMOS VLT deep survey VVDS-02h field

Author: P. Ciliegi, G. Zamorani, M. Bondi, L. Pozzetti, M. Bolzonella, L. Gregorini, B. Garilli, A. Iovino, H. J. McCracken, Y. Mellier, M. Radovich, H. R. de Ruiter, P. Parma, D. Bottini, V. Le Brun, O. Le Fèvre, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, M. Arnaboldi, S. Arnouts, S. Bardelli, A. Cappi, S. Charlot, T. Contini, S. Foucaud, P. Franzetti, L. Guzzo, O. Ilbert, B. Marano, C. Marinoni, G. Mathez, A. Mazure, B. Meneux, R. Merighi, P. Merluzzi, S. Paltani, A. Pollo, E. Zucca, A. Bongiorno, G. Busarello, I. Gavignaud, R. Pellò, V. Ripepi, D. Rizzo, 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), Ciliegi P., Zamorani G., Bondi M., Pozzetti L., Bolzonella M., Gregorini L., Garilli B., Iovino A., McCracken H. J., Mellier Y., Radovich M., de Ruiter H. R., Parma P., Bottini D., Le Brun V., Le Fèvre O., Maccagni D., Picat J. P., Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Cappi A., Charlot S., Contini T., Foucaud S., Franzetti P., Guzzo L., Ilbert O., Marano B., Marinoni C., Mathez G., Mazure A., Meneux B., Merighi R., Merluzzi P., Paltani S., Pollo A., Zucca E., Bongiorno A., Busarello G., Gavignaud I., Pellò R., Ripepi V., and Rizzo D.
Subjects: Physics, radio continuum: galaxies, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Hubble Deep Field, Astrophysics::High Energy Astrophysical Phenomena, Near-infrared spectroscopy, Flux, Astronomy and Astrophysics, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies: general, Galaxy, Redshift, Luminosity, Space and Planetary Science, cosmology: observations, 0103 physical sciences, Magnitude (astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift
Abstract: In this paper we present the optical and near-infrared identifications of the 1054 radio sources detected in the 20 cm deep radio survey down to a 5sigma flux limit of ~80 muJy obtained with the VLA in the VIMOS VLT Deep Survey VVDS-02h deep field. Using U,B,V,R,I and K data, with limiting magnitudes of UAB~25.4, BAB~26.5, VAB~26.2, RAB~25.9 IAB~25.0, JAB~24.2, KAB~23.9 (50% completeness) we identified 718 radio sources (~74% of the whole sample). The photometric redshift analysis shows that, in each magnitude bin, the radio sample has a higher median photometric redshift than the whole optical sample, while the median (V-I)AB color of the radio sources is redder than the median color of the whole optical sample. These results suggest that radio detection is preferentially selecting galaxies with higher intrinsic optical luminosity. From the analysis of the optical properties of the radio sources as function of the radio flux, we found that while about 35% of the radio sources are optically unidentified in the higher radio flux bin (S> 1.0 mJy), the percentage of unidentified sources decreases to about 25% in the faintest bins (S< 0.5 mJy). The median IAB magnitude for the total sample of radio sources, i.e. including also the unidentified ones, is brighter in the faintest radio bins than in the bin with higher radio flux. This suggests that most of the faintest radio sources are likely to be associated to relatively lower radio luminosity objects at relatively modest redshift, rather than radio-powerful, AGN type objects at high redshift. Using a classification in early-type and late-type galaxies based on the (B-I)AB color and the photometric redshift, we found that the majority of the radio sources below ~0.15 mJy are indeed late-type star forming galaxies. Finally, the radio sources without optical counterpart in our deep imaging have a median radio flux of 0.15 mJy, equal to that of identified sources. Given the very faint optical limits, these unidentified radio sources probably contain a significant fraction of obscured and/or high redshift galaxies.
Published: 2005
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36. Deep Redshift Surveys: The VIMOS VLT Deep Survey (Invited)

Author: D. Maccagni, S. Bardelli, S. Paltani, C. Adami, O. Le Fevre, D. Bottini, H. J. McCracken, E. Zucca, G. Vettlani, M. Arnoboldi, C. Marinoni, P. Merluzi, J. P. Picat, G. Mathez, Marco Scodeggio, V. Le Brun, R. Pello, O. Ilbert, B. Meneux, G. Busarello, A. Iovino, T. Contine, A. Zanichelli, Yannick Mellier, Alain Mazure, L. Tresse, R. Scaramella, Stephane Charlot, A. Cappi, I. Gavignaud, M. Radovich, Luigi Guzzo, G. Zamorani, and B. Garilli
Subjects: Physics, education.field_of_study, Galaxy type, Population, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, Luminosity, Magnitude (astronomy), Local environment, education, VIMOS-VLT Deep Survey, Astrophysics::Galaxy Astrophysics
Abstract: In this paper, the goals and methods of deep redshift surveys are reviewed and on-going projects are discussed. The requirements on instrumentation and observations methods are very stringent and call for a dedicated approach. Among the several on-going deep surveys, we are describing the VIMOS VLT Deep Survey (VVDS) which our team is conducting. It aims to obtain spectra in the redshift range 0 < z < 5, for a complete magnitude limited sample of more than 150000 galaxies. This will allow to quantify the evolution of the galaxy and AGN population over more than 90% of the current age of the universe, as a function of galaxy type, luminosity, or local environment.
Published: 2004
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37. Virmos-VLT deep survey (VVDS)

Author: G. Zamorani, E. Zucca, Sylvie Foucaud, Alain Mazure, Alessandro Zanichelli, Yannick Mellier, Roser Pello, Stéphane Colombi, Bianca Garilli, M. Scoreggio, Oliver Le Fevre, G. Mathez, J. P. Picat, Dario Mancini, P. Saracco, Roberto Scaramella, E. Bertin, M. Arnaboldi, M. Dantel-Fort, Laurence Tresse, Luigi Guzzo, S. Bardelli, A. Cappi, Christian Marinoni, G. Busarello, A. Iovino, D. Maccagni, Mario Radovich, V. Ripepi, Gianpaolo Vettolani, H. J. McCracken, Guido Chincarini, and Stéphane Charlot
Subjects: Physics, Galactic astronomy, Astrophysics::High Energy Astrophysical Phenomena, Near-infrared spectroscopy, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Galaxy, Observational cosmology, Magnitude (astronomy), Galaxy formation and evolution, Spectrograph, Astrophysics::Galaxy Astrophysics
Abstract: The Virmos-VLT deep survey (VVDS) is aimed to study the evolution of galaxies, large scale structure and AGNs over more than 90% of the current age of the Universe, based on a large number (more than 100.000) of spectra of galaxies. In a first step, the Vimos Spectrograph will be used to measure all galaxies from magnitude limited samples. In a second step, near IR spectroscopy will be obtained with the Nirmos spectrograph, to measure redshifts in the critical range 1.2 AB = 22.5. At the center of one region a deep survey will be conducted for galaxies brighter than I AB = 24. This deep region has also been imaged at the VLA (1400 MHz) to a flux limit of 0.08 mJy and is being observed in X-Rays with XMM.
Published: 2003
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38. VIMOS and NIRMOS multi-object spectrographs for the ESO VLT

Author: Bianca Garilli, Christian Lucuix, Enrico Cascone, Sandro D'Odorico, Bernard Delabre, Gert Finger, Gotthard Huster, Filippo Maria Zerbi, Oliver LeFevre, D. Maccagni, Luc Arnold, James W. Beletic, Gianpaolo Vettolani, Guy Monnet, J. P. Picat, L. Hill, Gerardo Avila, Javier Reyes Moreno, Michel Saisse, Pietro Schipani, Dario Mancini, Yannick Mellier, Paolo Conconi, Alain Mazure, E. Mattaini, Clothaire Voet, S. Brau-Nogué, Eric Prieto, Andree Laloge, Jean-Gabriel Cuby, Alan Moorwood, and G. Waultier
Subjects: Physics, Very Large Telescope, Optics, Galactic astronomy, business.industry, Astronomy, First light, Spectral resolution, business, Redshift survey, Spectrograph, Galaxy, Redshift
Abstract: The VIRMOS consortium of French and Italian Institutes is manufacturing 2 wide field imaging multi-object spectrographs for the European Southern Observatory Very Large Telescope, with emphasis on the ability to carry over spectroscopic surveys of large numbers of sources. The Visible Multi-Object Spectrograph, VIMOS, is covering the 0.37 to 1 micron wavelength domain, with a full field of view of 4 by 7 by 8 arcmin 2 in imaging and MOS mode. The Near IR Multi-Object Spectrograph, NIRMOS, is covering the 0.9 to 1.8 microns wavelength range, with afield of view 4 by 6 by 8 arcmin 2 in MOS mode. The spectral resolution for both instrument scan reach up to R equals 5000 for a 0.5 arcsec wide slit. Multi-slit masks are produced by a dedicated Mask Manufacturing Machine cutting through thin Invar sheets and capable of producing 4 slit masks approximately 300 by 300 mm each with approximately slits 5.7 mm long in less than one hour. Integral field spectroscopy is made possible in VIMOS by switching in the beam specially build masks fed by 6400 fibers coming form a 54 by 54 arcsec 2 integral field head with a 80 by 80 array of silica micro-lenses. NIRMOS has a similar IFS unit with a field of 30 by 30 arcmin 2 . These instruments are designed to offer very large multiplexing capabilities. In MOS mode, about 1000 objects can be observed simultaneously with VIMOS, with a S/N equals 10 obtained on galaxies with I equals 24 in one hour, and approximately 200 objects can be observed simultaneously with NIRMOS, with a S/N equals 10 obtained don galaxies with J equals 22, H equals 20.6 in 1h at R eq equals 200. We present here the status of VIMOS, currently under final integration, with expected first light in the summer 2000, together with the final design of NIRMOS presented at the Final Design Review. The VLT-VIRMOS deep redshift survey of more with the final design of NIRMOS presented at the Final Design Review. The VLT-VIRMOS deep redshift survey of more than 150000 galaxies over the redshift range 0 < z < 5 will be undertaken based on 120 guaranteed nights awarded to the project.
Published: 2000
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39. EMIR, cryogenic NIR multi-object spectrograph for GTC

Author: Rafael Guzman, N. Cardiel, J. Azcue, Alfonso Aragón-Salamanca, David J. Robertson, Dave Carter, Damien Jones, Reynier Peletier, Francis Beigbeder, Fernando Gago, Antonio Manescau, Marc Balcells, Ana Belen Fragoso-Lopez, Ray M. Sharples, S. Brau-Nogué, Peter Luke, T. Munoz, Juan Carlos López, J. C. Heredero, E. de la Fuente, Roser Pello, M. T. Barroso, Jose J. Diaz-Garcia, Jose Alberto Ballester Lluch, F. Javier Fuentes, J. Gomez-Elvira, J. Patrón, Ángel Serrano, José Antonio Lozano Rodríguez, J. P. Picat, Jaime Zamorano, and J. Gallego
Subjects: Physics, Design phase, Astrofísica, Astronomía, Galactic astronomy, Spectrometer, Near-infrared spectroscopy, Astronomy, Field of view, Astrophysics, Object (computer science), Spectrograph, Galaxy
Abstract: EMIR is a near-IR, multi-slit camera-spectrograph under development for the 10m GTC on La Palma. It will deliver up to 45 independent R equals 3500-4000 spectra of sources over a field of view of 6 feet by 3 feet, and allow NIR imaging over a 6 foot by 6 foot FOV, with spatial sampling of 0.175 inch/pixel. The prime science goal of the instrument is to open K-band, wide field multi-object spectroscopy on 10m class telescopes. Science applications range from the study of star-forming galaxies beyond z equals 2, to observations of substellar objects and dust-enshrouded star formation regions. Main technological challenges include the large optics, the mechanical and thermal stability and the need to implement a mask exchange mechanism that does not require warming up the spectrograph. EMIR is begin developed by the Instituto de Astrofisica de Canarias, the Instituto Nacional de Tecnica Aeroespacial, the Universidad Complutense de Madrid, the Observatoire Midi-Pyrennees, and the University of Durham. Currently in its Preliminary Design phase, EMIR is expected to start science operation in 2004.
Published: 2000

40. VIRMOS: Deep Redshift Surveys with the VLT

Author: D. Maccagni, Dario Mancini, P. Vettolani, Jean-Gabriel Cuby, Alain Mazure, O. Le Fèvre, J. P. Picat, and Yannick Mellier
Subjects: Physics, Star formation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, First light, Redshift survey, Galaxy, Redshift, Visible infrared, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Spectrograph, Astrophysics::Galaxy Astrophysics
Abstract: We present the status of the feasibility study of the Visible InfraRed Multi Object Spectrograph, conducted under contract with ESO for the VLT. The aim of this study is to establish the scientific objectives, identify the opto-mechanical concepts, and predict the performances of a wide-field multi-object spectrograph dedicated to the deepest galaxy and AGN redshift surveys that will be possible with the VLT. We have identified that a concept based on a four quadrant imaging-spectrograph, using multi-slit aperture plates, is the most efficient concept in this context. The maximum number of slits 10 arcseconds in length, that can be observed simultaneously, is in excess of 800, offering a spectacular multiplexing gain in a field of 4 × 7 × 8 arcmin2, for a wavelength coverage from 0.37 to 1.8μm. We are proposing a dedicated wide-field deep redshift survey, to collect ~ 105 galaxies brighter than I = 24, in the redshift range 0.3 4 or more, in less than 200 nights at one Nasmyth focus of the VLT. The timescale of the instrument development is expected to be 4 years, with first light in early 2001, provided that the VIRMOS concept is selected by ESO early in 1997.
Published: 1997
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41. The VLT-VIRMOS Deep Redshift Survey

Author: Jean-Gabriel Cuby, Dario Mancini, Alain Mazure, J. P. Picat, O. Le Fèvre, Yannick Mellier, D. Maccagni, and P. Vettolani
Subjects: Physics, Visible infrared, Astrophysics::Instrumentation and Methods for Astrophysics, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Astronomy, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift survey, Spectrograph, Astrophysics::Galaxy Astrophysics, Galaxy, Luminosity function
Abstract: VIRMOS, the Visible InfraRed Multi Object Spectrograph, is being studied under contract with ESO, to identify the opto-mechanical concepts, and predict the performances of a wide-field multi-object spectrograph dedicated to the deepest galaxy, large scale
Published: 1997
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42. 'Va-et-Vient' ('Back-and-Forth') CCD Spectroscopy: A New Way to Increase the Limiting Magnitude of Very Large Telescopes

Author: J. P. Picat, B. Fort, J. C. Cuillandre, and G. Soucail
Subjects: Physics, media_common.quotation_subject, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift, Galaxy, Universe, Photometry (astronomy), Sky, Limiting magnitude, Magnitude (astronomy), Galaxy formation and evolution, Astrophysics::Galaxy Astrophysics, media_common
Abstract: Over the last decade, the quantity of scientific results brought by the observations of very faint objects has been quite spectacular. In particular, they concern the photometry of faint galaxies up to B = 27 (Tyson 1988) or K = 22 (Cowie et al. 1994). The consequences of these observations are the detection of a large population of faint galaxies more numerous than any prediction given by standard galaxy evolution and probably a new vision of the distant universe. For faint object spectroscopy, the most recent surveys of field galaxies reach a magnitude range of 23–24 (Colless et al. 1990, 1993, Lilly and Cowie 1993, Tresse et al. 1993) with a reasonable S/N ratio that allows a redshift measurement from absorption-line identification. But in this magnitude range, the sky background flux is dominant with respect to the source, being at least 10 times brighter. It is well known that in that case, with a low readout noise detector and a “perfect” spectrograph, the S/N ratio scales as
Published: 1995
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43. Early results from the VIMOS VLT Deep Survey

Author: V. Le Brun, O. Ilbert, G. Mathez, H. J. McCracken, G. Zamorani, Alain Mazure, D. Bottini, Stéphane Charlot, M. Bolzonella, O. Le Fevre, R. Pello, Mario Radovich, I. Gavignaud, A. Iovino, Bruno Marano, A. Cappi, Lucia Pozzetti, P. Franzetti, B. Meneux, S. Paltani, Roberto Scaramella, Sylvie Foucaud, C. Adami, Paolo Ciliegi, Christian Marinoni, B. Garilli, Luigi Guzzo, Paola Merluzzi, T. Contini, A. Pollo, S. Bardelli, Marco Scodeggio, G. Busarello, D. Maccagni, E. Zucca, D. Rizzo, L. Tresse, G. Vettolani, A. Zanichelli, Magda Arnaboldi, M. Bondi, J. P. Picat, Yannick Mellier, MATTHEW COLLESS, LISTER STAVELEY-SMITH AND RAYLEE STATHAKIS., Le Fèvre O., Adami C., Ilbert O., Le Brun V., Marinoni C., Mazure A., Meneux B., Paltani S., Tresse L., Vettolani G., Bondi M., Cappi A., Ciliegi P., Marano B., McCracken H. J., Pozzetti L., Zanichelli A., Maccagni D., Bottini D., Foucaud S., Franzetti P., Garilli B., Scodeggio M., Picat J. P., Contini T., Gavignaud I., Mathez G., Pellò R., Arnaboldi M., Busarello G., Merluzzi P., Radovich M., Mellier Y., Charlot S., Guzzo L., Iovino A., Pollo A., Rizzo D., Scaramella R., Bardell S., Bolzonelle M., Zamorani G., and Zucca E.
Subjects: Physics, Wavelength range, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift, Galaxy, Spectral line, Early results, Magnitude (astronomy), VIMOS-VLT Deep Survey, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract: The VIMOS VLT Deep Survey (VVDS) is underway to study the evolution of galaxies, large scale structures and AGNs, from the measurement of more than 100000 spectra of faint objects. We present here the results from the first epoch observations of more than 20000 spectra. The main challenge of the program, the redshift measurements, is described, in particular entering the ``redshift desert'' in the range $1.5, Comment: 8 pages, 7 figures, in the proceedings of IAU Symposium 216 "Maps of the Cosmos", Sydney, July 2003, M. Colless & L. Staveley-Smith Eds

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