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101. 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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102. Comparison of the VIMOS-VLT Deep Survey with the Munich semi-analytical model : I. Magnitude counts, redshift distribution, colour bimodality, and galaxy clustering

Author

S. de la Torre, B. Meneux, G. De Lucia, J. Blaizot, O. Le Fèvre, B. Garilli, O. Cucciati, Y. Mellier, A. Pollo, U. Abbas, D. Bottini, V. Le Brun, D. Maccagni, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, 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, C. Marinoni, A. Mazure, R. Merighi, S. Paltani, R. Pelló, L. Pozzetti, D. Vergani, G. Zamorani, E. Zucca, S. de la Torre, B. Meneux, G. De Lucia, J. Blaizot, O. Le Fèvre, B. Garilli, O. Cucciati, Y. Mellier, A. Pollo, U. Abba, D. Bottini, V. Le Brun, D. Maccagni, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnout, 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, C. Marinoni, A. Mazure, R. Merighi, S. Paltani, R. Pelló, L. Pozzetti, D. Vergani, G. Zamorani, and E. Zucca

Subjects
statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Universe, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, 10. No inequality, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies], Physics, cosmology: observation, galaxies, 010308 nuclear & particles physics, Astronomy and Astrophysics, large-scale structure of, Redshift, Galaxy, observations [cosmology], Bimodality, Distribution (mathematics), statistics, Space and Planetary Science, Magnitude (astronomy), large-scale structure of Universe, galaxies: evolution, VIMOS-VLT Deep Survey, high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This paper presents a detailed comparison between high-redshift observations from the VIMOS-VLT Deep Survey (VVDS) and predictions from the Munich semi-analytical model of galaxy formation. In particular, we focus this analysis on the magnitude, redshift, and colour distributions of galaxies, as well as their clustering properties. We constructed 100 quasi-independent mock catalogues, using the output of the semi-analytical model presented in De Lucia & Blaizot (2007).We then applied the same observational selection function of the VVDS-Deep survey, so as to carry out a fair comparison between models and observations. We find that the semi-analytical model reproduces well the magnitude counts in the optical bands. It tends, however, to overpredict the abundance of faint red galaxies, in particular in the i' and z' bands. Model galaxies exhibit a colour bimodality that is only in qualitative agreement with the data. In particular, we find that the model tends to overpredict the number of red galaxies at low redshift and of blue galaxies at all redshifts probed by VVDS-Deep observations, although a large fraction of the bluest observed galaxies is absent from the model. In addition, the model overpredicts by about 14 per cent the number of galaxies observed at 0.2, Comment: 15 pages, 14 figures, accepted for publication in A&A

Published
2011

103. The Star Formation Rate Density and Dust Attenuation Evolution over 12 Gyr with the VVDS Surveys

Author

E. Zucca, Daniela Vergani, O. Le Fèvre, Micol Bolzonella, G. Zamorani, Bianca Garilli, M. Scodeggio, D. Maccagni, V. Le Brun, Paolo Cassata, H. J. McCracken, P. Franzetti, A. Zanichelli, S. Bardelli, L. Tresse, R. M. Bielby, Olga Cucciati, Olivier Ilbert, O. Cucciati, L. Tresse, O. Ilbert, O. Le Fèvre, B. Garilli, V. Le Brun, P. Cassata, P. Franzetti, D. Maccagni, M. Scodeggio, E. Zucca, G. Zamorani, S. Bardelli, M. Bolzonella, R. M. Bielby, H. J. McCracken, A. Zanichelli, D. Vergani, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Absolute magnitude, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Cosmology: observations, Galaxies: evolution, Galaxies: high-redshift, Galaxies: luminosity function, mass function, Galaxies: star formation, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, cosmology: observation, 010308 nuclear & particles physics, Star formation, Redshift survey, Galaxy, Redshift, Stars, galaxies: luminosity function, mass function, galaxies: star formation, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

[Abridged] We investigate the global galaxy evolution over 12 Gyr (0.051.7, we set alpha steepening with (1+z). The absolute magnitude M*_FUV brightens in the entire range 02 it is on average brighter than in the literature, while phi* is smaller. Our total LD shows a peak at z=2, present also when considering all sources of uncertainty. The SFRD history peaks as well at z=2. It rises by a factor of 6 during 2 Gyr (from z=4.5 to z=2), and then decreases by a factor of 12 during 10 Gyr down to z=0.05. This peak is mainly produced by a similar peak within the population of galaxies with -21.52 of the SFRD is compelling for models of galaxy formation. The mean dust attenuation A_FUV of the global galaxy population rises by 1 mag during 2 Gyr from z=4.5 to z=2, reaches its maximum at z=1 (A_FUV=2.2 mag), and then decreases by 1.1 mag during 7 Gyr down to z=0. The dust attenuation maximum is reached 2 Gyr after the SFRD peak, implying a contribution from the intermediate-mass stars to the dust production at z, Comment: 23 pages, 15 figures, accepted for publication in A&A

Published
2011
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104. The VIMOS VLT Deep Survey: star formation rate density of Lyα emitters from a sample of 217 galaxies with spectroscopic redshifts 2 ≤ z ≤ 6.6

Author

E. Zucca, A. Zanichelli, Paolo Cassata, Lucia Pozzetti, H. J. McCracken, A. Cappi, L. Tresse, R. M. Bielby, Olga Cucciati, D. Maccagni, B. Garilli, O. Le Fevre, Daniela Vergani, A. Pollo, G. Zamorani, S. Bardelli, Marco Scodeggio, Yannick Mellier, Thierry Contini, V. Le Brun, O. Ilbert, 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), P. Cassata, O. Le Fèvre, B. Garilli, D. Maccagni, V. Le Brun, M. Scodeggio, L. Tresse, O. Ilbert, G. Zamorani, O. Cucciati, T. Contini, R. Bielby, Y. Mellier, H. J. McCracken, A. Pollo, A. Zanichelli, S. Bardelli, A. Cappi, L. Pozzetti, D. Vergani, and E. Zucca

Subjects
cosmology: observations, galaxies: evolution, galaxies: formation, galaxies: fundamental parameters, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, Galaxy formation and evolution, [INFO]Computer Science [cs], Emission spectrum, 010303 astronomy & astrophysics, galaxies: fundamental parameter, ComputingMilieux_MISCELLANEOUS, Line (formation), Luminosity function (astronomy), Physics, cosmology: observation, 010308 nuclear & particles physics, Star formation, Redshift, Galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Aims. The aim of this work is to study the contribution of the Ly-a emitters (LAE) to the star formation rate density (SFRD) of the Universe in the interval 21.5x10^18 erg/s/cm^2 are 33 galaxies/arcmin^2 and 4x10^-2 Mpc^-3, respectively. We find that the the observed luminosity function of LAE does not evolve from z=2 to z=6. This implies that, after correction for the redshift-dependent IGM absorption, the intrinsic LF must have evolved significantly over 3 Gyr. The SFRD from LAE contributes to about 20% of the SFRD at z =2-3, while the LAE appear to be the dominant source of star formation producing ionizing photons in the early universe z>5-6, becoming equivalent to that of Lyman Break galaxies., Comment: 17 pages, 20 figures, accepted for publication to A&A

Published
2011
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105. XMM-Newtonobservation of the interacting cluster Abell 3528

Author

E. Zucca, Silvano Molendi, S. Bardelli, Fabio Gastaldello, Tiziana Venturi, and Stefano Ettori

Subjects
Physics, media_common.quotation_subject, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Universe, Redshift, Core (optical fiber), Space and Planetary Science, Supercluster, Cluster (physics), Surface brightness, Galaxy cluster, media_common
Abstract

We analyze the XMM dataset of the interacting cluster of galaxies Abell 3528 located westward in the core of the Shapley Supercluster, the largest concentration of mass in the nearby Universe. A3528 is formed by two interacting clumps (A3528-N at North and A3528-S at South) separated by 0.9 $h_{70}^{-1}$ Mpc at redshift 0.053. XMM data describe these clumps as relaxed structure with an overall temperature of $4.14 \pm 0.09$ and $4.29 \pm 0.07$ keV in A3528-N and A3528-S, respectively, and a core cooler by a factor 1.4--1.5 and super-solar metal abundance in the inner 30 arcsec. These clumps are connected by a X-ray soft, bridge-like emission and present asymmetric surface brightness with significant excess in the North--West region of A3528-N and in the North--East area of A3528-S. However, we do not observe any evidence of shock heated gas, both in the surface brightness and in the temperature map. Considering also that the optical light distribution is more concentrated around A3528-N and makes A3528-S barely detectable, we do not find support to the originally suggested head-on pre-merging scenario and conclude that A3528 is in a off-axis post-merging phase, where the closest cores encounter happened about 1--2 Gyrs ago., Comment: 15 pages, 16 figures (10 in colors), accepted for publication on A&A. For a Poscript version with high resolution figures see http://www.mi.iasf.cnr.it/~gasta/www/a3528.html

Published
2003
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106. The origin of X-ray emission of two distant ($\mathsf{\textit{z}\,>1}$) cluster candidates with XMM-Newton

Author

E. Zucca, Stephane Arnouts, L. F. Olsen, H. E. Jørgensen, Doris M. Neumann, Andrea Biviano, S. Bardelli, M. Arnaud, C. Benoist, M. Ramella, and L. N. da Costa

Subjects
Physics, Space and Planetary Science, Near-infrared spectroscopy, Center (category theory), Cluster (physics), Astronomy and Astrophysics, Astrophysics, Lambda, Galaxy, Galaxy cluster, Redshift, Luminosity
Abstract

We present here a study of XMM-Newton data of two distant galaxy cluster candidates. One of these was discovered serendipitously in near infrared data, CL J0533-2411, the other one corresponds to the cluster EIS J0533-2412 part of the EIS cluster survey. The estimated redshift of CL J0533-2411 is z=1.2-1.7. EIS J0533-2412 is a rich system (Lambda_cl=299), with a spectroscopically confirmed redshift of z=1.3. Both galaxy concentrations show firm X-ray detections, located within 30" of their optical center. However, we cannot resolve the sources with XMM-Newton. If the X-ray emission originates from the X-ray emitting intra-cluster medium (ICM) it would be extremely concentrated which is rather unlikely (core radii below 14 h_{65}^{-1}kpc and 40 h_{65}^{-1}kpc, respectively). We argue that the X-ray sources are more likely AGN members of the galaxy concentrations. We set an upper limit for the bolometric luminosity of a hot ICM in the range ~0.7-2.1 10^{44} h_{65}^{-2}erg/s for CL J0533-2411, depending on the exact redshift. For EIS J0533-2412 the limit is L_bol=(6.2+/-1.4) 10^{43} h_{65}^{-2}erg/s. We interpret our result in the following way: EIS J0533-2412 (and possibly CL J0533-2411) are proto-clusters and show matter overdensities before collapse, which explains the low significance of extended X-ray emission.

Published
2003
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107. Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelength Spitzer observations up to z ~ 2.5

Author

Micol Bolzonella, S. de la Torre, Paola Santini, Alberto Franceschini, M. Bondi, Adriano Fontana, Mattia Vaccari, E. Zucca, Giulia Rodighiero, L. Tresse, V. Le Brun, Olivier Ilbert, G. Zamorani, Bianca Garilli, S. Bardelli, Andrea Grazian, D. L. Shupe, I. Matute, O. Le Fèvre, Daniela Vergani, C. Mancini, Andrea Cimatti, Carol J. Lonsdale, Lucia Pozzetti, Jason Surace, S. Arnouts, Lucia Marchetti, Michael Rowan-Robinson, 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), G. Rodighiero, M. Vaccari, A. Franceschini, L. Tresse, O. Le Fevre, V. Le Brun, C. Mancini, I. Matute, A. Cimatti, L. Marchetti, O. Ilbert, S. Arnout, M. Bolzonella, E. Zucca, S. Bardelli, C. J. Lonsdale, D. Shupe, J. Surace, M. Rowan-Robinson, B. Garilli, G. Zamorani, L. Pozzetti, M. Bondi, S. de la Torre, D. Vergani, P. Santini, A. Grazian, and A . Fontana

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, infrared: galaxies, Far infrared, surveys, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, COSMIC cancer database, Number density, 010308 nuclear & particles physics, Astronomy and Astrophysics, galaxies: fundamental parameters, Galaxy, Redshift, Stars, galaxies: luminosity function, 13. Climate action, Space and Planetary Science, mass function, cosmology: observations, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

[Abridged]We exploit a large homogeneous dataset to derive a self-consistent picture of IR emission based on the time-dependent 24, 15, 12 and 8micron monochromatic and bolometric IR luminosity functions (LF) over the 01. The mean redshift of the peak in the source number density shifts with luminosity: the brighest IR galaxies appear to be forming stars earlier in cosmic time (z>1.5), while the less luminous ones keep doing it at more recent epochs (z~1 for L(IR)1. We also seem to find a difference in the evolution rate of the source number densities as a function of luminosity, a downsizing evolutionary pattern similar to that reported from other samples of cosmic sources., Comment: Accepted for pubblicantion in Astronomy and Astrophysics

Published
2010
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108. zCOSMOS - 10k-bright spectroscopic sample. The bimodality in the Galaxy Stellar Mass Function: exploring its evolution with redshift

Author

L. Pozzetti, M. Bolzonella, E. Zucca, G. Zamorani, S. Lilly, A. Renzini, M. Moresco, M. Mignoli, P. Cassata, L. Tasca, F. Lamareille, C. Maier, B. Meneux, C. Halliday, P. Oesch, D. Vergani, K. Caputi, K. Kovač, A. Cimatti, O. Cucciati, A. Iovino, Y. Peng, M. Carollo, T. Contini, J.-P. Kneib, O. Le Févre, V. Mainieri, M. Scodeggio, S. Bardelli, A. Bongiorno, G. Coppa, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, P. Kampczyk, C. Knobel, J.-F. Le Borgne, V. Le Brun, R. Pellò, E. Perez Montero, E. Ricciardelli, J. D. Silverman, M. Tanaka, L. Tresse, U. Abbas, D. Bottini, A. Cappi, L. Guzzo, A. M. Koekemoer, A. Leauthaud, D. Maccagni, C. Marinoni, H. J. McCracken, P. Memeo, C. Porciani, R. Scaramella, C. Scarlata, N. Scoville, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Università di Bologna, Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), INAF - Osservatorio Astronomico di Brera (OAB), AUTRES, 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 Astrofisico di Arcetri (OAA), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Physics and Astronomy [UCLA Los Angeles], University of California [Los Angeles] (UCLA), University of California-University of California, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, INAF- Milano, Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Glycosciences Laboratory, Imperial College School of Medicine, Tokai University, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), California Institute of Technology (CALTECH), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), University of California (UC)-University of California (UC), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), L. Pozzetti, M. Bolzonella, E. Zucca, G. Zamorani, S. Lilly, A. Renzini, M. Moresco, M. Mignoli, P. Cassata, L. Tasca, F. Lamareille, C. Maier, B. Meneux, C. Halliday, P. Oesch, D. Vergani, K. Caputi, K. Kovac, A. Cimatti, O. Cucciati, A. Iovino, Y. Peng, M. Carollo, T. Contini, J.P. Kneib, O. Le F'evre, V. Mainieri, M. Scodeggio, S. Bardelli, A. Bongiorno, G. Coppa, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, P. Kampczyk, C. Knobel, J.F. Le Borgne, V. Le Brun, R. Pell`o, E. Perez Montero, E. Ricciardelli, J.D. Silverman, M. Tanaka, L. Tresse, U. Abba, D. Bottini, A. Cappi, L. Guzzo, A.M. Koekemoer, A. Leauthaud, D. Maccagni, C. Marinoni, H.J. McCracken, P. Memeo, C. Porciani, R. Scaramella, C. Scarlata, N. Scoville, and Astronomy

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), EXTREMELY RED GALAXIES, Stellar mass, EARLY DATA RELEASE, galaxies: evolution, galaxies: formation, galaxies: luminosity function, mass function, galaxies: statistics, Astronomy and Astrophysics, Space and Planetary Science, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, SIMILAR-TO 1, 01 natural sciences, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, FORMATION HISTORY, education.field_of_study, Number density, Spiral galaxy, 010308 nuclear & particles physics, Star formation, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], VLT DEEP SURVEY, DISK GALAXIES, Redshift, Galaxy, COSMOS FIELD, Stars, galaxies: luminosity function, LUMINOSITY FUNCTION, mass function, DIGITAL SKY SURVEY, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the Galaxy Stellar Mass Function (MF) up to z~1 from the zCOSMOS-bright 10k spectroscopic sample. We investigate the total MF and the contribution of ETGs and LTGs, defined by different criteria (SED, morphology or star formation). We unveil a galaxy bimodality in the global MF, better represented by 2 Schechter functions dominated by ETGs and LTGs, respectively. For the global population we confirm that low-mass galaxies number density increases later and faster than for massive galaxies. We find that the MF evolution at intermediate-low values of Mstar (logM, Revised version, accepted for publication on Astronomy and Astrophysics

Published
2010
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109. The very steep spectrum radio halo in Abell 697

Author

Gianfranco Brunetti, S. Bardelli, R. Athreya, Daniele Dallacasa, Simona Giacintucci, Giulia Macario, Rossella Cassano, Tiziana Venturi, G. Macario, T. Venturi, G. Brunetti, D. Dallacasa, S. Giacintucci, R. Cassano, S. Bardelli, and R. Athreya

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, RADIATION MECHANISM: NON-THERMAL, Order (ring theory), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Low frequency, Radio spectrum, Galaxy, GALAXIES: CLUSTERS: INDIVIDUAL: ABELL 697, GALAXIES: CLUSTERS: GENERAL, Radio halo, Space and Planetary Science, Cluster (physics), Halo, Energy (signal processing), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In this paper we present a detailed study of the giant radio halo in the galaxy cluster Abell 697, with the aim to constrain its origin and connection with the cluster dynamics. We performed high sensitivity GMRT observations at 325 MHz, which showed that the radio halo is much brighter and larger at this frequency, compared to previous 610 MHz observations. In order to derive the integrated spectrum in the frequency range 325 MHz--1.4 GHz, we re--analysed archival VLA data at 1.4 GHz and made use of proprietary GMRT data at 610 MHz. {Our multifrequency analysis shows that the total radio spectrum of the giant radio halo in A\,697 is very steep, with $\alpha_{\rm~325 MHz}^{\rm~1.4 GHz} \approx 1.7-1.8$. %\pm0.1$. Due to energy arguments, a hadronic origin of the halo is disfavoured by such steep spectrum. Very steep spectrum halos in merging clusters are predicted in the case that the emitting electrons are accelerated by turbulence, observations with the upcoming low frequency arrays will be able to test these expectations.}, Comment: 10 pages, 8 figures, A&A in press

Published
2010
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110. The VIMOS ultra-deep survey: 10 000 galaxies with spectroscopic redshifts to study galaxy assembly at early epochs 2 < z ≃ 6

Author

Stéphane Charlot, O. Cucciati, S. de la Torre, G. Zamorani, Peter Capak, Yannick Mellier, Jean-Gabriel Cuby, E. Zucca, Laura Pentericci, V. Sommariva, A. Grazian, Marco Scodeggio, V. Le Brun, L. A. M. Tasca, Olivier Ilbert, Rajat M. Thomas, A. Durkalec, Ricardo Amorín, M. Castellano, P. W. Wang, Mara Salvato, D. Vergani, Letizia P. Cassarà, O. Le Fevre, Daniel Schaerer, Paolo Cassata, A. Cimatti, T. Contini, C. Moreau, E. Vanzella, Brian Lemaux, B. Garilli, S. Bardelli, Adriano Fontana, Yoshiaki Taniguchi, C. Lopez-Sanjuan, Nick Scoville, L. Tresse, M. Giavalisco, S. Fotopoulo, Nimish P. Hathi, Margherita Talia, D. Maccagni, Stéphane Paltani, B. Ribeiro, Le Fèvre, O., Tasca, L.A.M., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zamorani, G., Zucca, E., Amorin, R., Bardelli, S., Capak, P., Cassarà, L., Castellano, M., Cimatti, A., Cuby, J.G., Cucciati, O., De La Torre, S., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Lemaux, B.C., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.W., Charlot, S., Contini, T., Fotopoulou, S., López-Sanjuan, C., Mellier, Y., Scoville, N., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Stellar mass, Large-scale structure of Universe, Population, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Galaxies: formation, Lambda, Cosmology: observation, Spectral line, Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], education, Survey, Astrophysics::Galaxy Astrophysics, Cosmology: observations, Galaxies: evolution, Galaxies: high-redshift, Astronomy and Astrophysics, Space and Planetary Science, Physics, education.field_of_study, Star formation, Astronomy and Astrophysic, Redshift survey, Redshift, Galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the VIMOS Ultra Deep Survey (VUDS), a spectroscopic redshift survey of ~10.000 very faint galaxies to study the major phase of galaxy assembly 2, Comment: 43 pages, 30 figures, submitted to A&A

Published
2015
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111. Brightest Cluster Galaxies in the Extended GMRT radio halo cluster sample. Radio properties and cluster dynamics

Author

Tiziana Venturi, E. Zucca, Daniele Dallacasa, Simona Giacintucci, Ruta Kale, S. Bardelli, Rossella Cassano, Kale, R., Venturi, T., Cassano, R., Giacintucci, S., Bardelli, S., Dallacasa, D., and Zucca, E.

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Galaxies: active, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy and Astrophysic, Radio continuum: galaxie, X-rays: galaxies: cluster, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Luminosity, Radio halo, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Cluster (physics), Elliptical galaxy, Galaxies: clusters: general, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Luminosity function (astronomy)
Abstract

Brightest Cluster Galaxies (BCGs) show exceptional properties over the whole electromagnetic spectrum. Their special location at the centres of galaxy clusters raises the question of the role of the environment on their radio properties. To decouple the effect of the galaxy mass and of the environment in their statistical radio properties, we investigate the possible dependence of the occurrence of radio loudness and of the fractional radio luminosity function on the dynamical state of the hosting cluster. We studied the radio properties of the BCGs in the Extended GMRT Radio Halo Survey (EGRHS). We obtained a statistical sample of 59 BCGs, which was divided into two classes, depending on the dynamical state of the host cluster, i.e. merging (M) and relaxed (R). Among the 59 BCGs, 28 are radio-loud, and 31 are radio--quiet. The radio-loud sources are located favourably located in relaxed clusters (71\%), while the reverse is true for the radio-quiet BCGs, mostly located in merging systems (81\%). The fractional radio luminosity function (RLF) for the BCGs is considerably higher for BCGs in relaxed clusters, where the total fraction of radio loudness reaches almost 90\%, to be compared to the $\sim$30\% in merging clusters. For relaxed clusters, we found a positive correlation between the radio power of the BCGs and the strength of the cool core, consistent with previous studies on local samples. Our study suggests that the radio loudness of the BCGs strongly depends on the cluster dynamics, their fraction being considerably higher in relaxed clusters. We compared our results with similar investigations, and briefly discussed them in the framework of AGN feedback., Comment: 12 pages, 6 figures, 3 tables, A&A accepted

Published
2015
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112. Stellar mass to halo mass relation from galaxy clustering in VUDS: A high star formation efficiency at z ≠3 â†

Author

O. Cucciati, Yannick Mellier, S. de la Torre, A. Grazian, Paolo Cassata, Rajat M. Thomas, Marco Scodeggio, A. Cimatti, M. Giavalisco, Y. Taniguchi, D. Maccagni, Janine Pforr, E. Zucca, M. Castellano, Mara Salvato, V. Sommariva, C. Lopez-Sanjuan, Nick Scoville, G. Zamorani, A. Pollo, E. Vanzella, J. G. Cuby, James Dunlop, Daniel Schaerer, Ricardo Amorín, S. Bardelli, D. Vergani, Adriano Fontana, Peter Capak, T. Contini, L. A. M. Tasca, Sotiria Fotopoulou, Laura Pentericci, Anton M. Koekemoer, Margherita Talia, Stéphane Charlot, Brian Lemaux, B. Ribeiro, A. Durkalec, O. Le Fevre, Letizia P. Cassarà, P. W. Wang, Nimish P. Hathi, L. Tresse, V. Le Brun, O. Ilbert, S. Paltani, B. Garilli, Durkalec, A., Le Fèvre, O., De La Torre, S., Pollo, A., Cassata, P., Garilli, B., Le Brun, V., Lemaux, B.C., Maccagni, D., Pentericci, L., Tasca, L.A.M., Thomas, R., Vanzella, E., Zamorani, G., Zucca, E., Amorín, R., Bardelli, S., Cassarà, L.P., Castellano, M., Cimatti, A., Cucciati, O., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Paltani, S., Ribeiro, B., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vergani, D., Capak, P., Charlot, S., Contini, T., Cuby, J.G., Dunlop, J., Fotopoulou, S., Koekemoer, A., López-Sanjuan, C., Mellier, Y., Pforr, J., Salvato, M., Scoville, N., Taniguchi, Y., and Wang, P.W.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Large-scale structure of Universe, statistical [methods], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Halo occupation distribution, Early Universe, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Galaxies: evolution, Methods: statistical, Astronomy and Astrophysics, Space and Planetary Science, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, early Universe, Mass ratio, Astronomy and Astrophysic, Galaxy, Dark matter halo, Stars, large-scale structure of Universe, Astrophysics::Earth and Planetary Astrophysics, Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The relation between the galaxy stellar mass M_star and the dark matter halo mass M_h gives important information on the efficiency in forming stars and assembling stellar mass in galaxies. We present the stellar mass to halo mass ratio (SMHR) measurements at redshifts 2, Comment: 4 pages, 2 figures, submitted to A&A

Published
2015

113. Evolution of clustering length, large-scale bias, and host halo mass at 2 < z < 5 in the VIMOS Ultra Deep Survey (VUDS)

Author

A. Durkalec, O. Le Fèvre, A. Pollo, S. de la Torre, P. Cassata, B. Garilli, V. Le Brun, B. C. Lemaux, D. Maccagni, L. Pentericci, L. A. M. Tasca, R. Thomas, E. Vanzella, G. Zamorani, E. Zucca, R. Amorín, S. Bardelli, L. P. Cassarà, M. Castellano, A. Cimatti, O. Cucciati, A. Fontana, M. Giavalisco, A. Grazian, N. P. Hathi, O. Ilbert, S. Paltani, B. Ribeiro, D. Schaerer, M. Scodeggio, V. Sommariva, M. Talia, L. Tresse, D. Vergani, P. Capak, S. Charlot, T. Contini, J. G. Cuby, J. Dunlop, S. Fotopoulou, A. Koekemoer, C. López-Sanjuan, Y. Mellier, J. Pforr, M. Salvato, N. Scoville, Y. Taniguchi, P. W. Wang, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), AUTRES, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Oncology Institute of Southern Switzerland, INAF - Osservatorio Astronomico di Bologna (OABO), University of Bologna, Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], INAF- Milano, INAF - Osservatorio Astrofisico di Arcetri (OAA), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), SUPA, Institute for Astronomy, University of Edinburgh, Aristotle University of Thessaloniki, Space Telescope Science Institute (STSci), 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), Institute of cosmology and gravitation, University of Portsmouth, Max-Planck-Institut für Extraterrestrische Physik (MPE), California Institute of Technology (CALTECH), ANR-11-IDEX-0001,Amidex,INITIATIVE D'EXCELLENCE AIX MARSEILLE UNIVERSITE(2011), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Durkalec, A., Le Fevre, O., Pollo, A., De La Torre, S., Cassata, P., Garilli, B., Le Brun, V., Lemaux, B.C., Maccagni, D., Pentericci, L., Tasca, L.A.M., Thomas, R., Vanzella, E., Zamorani, G., Zucca, E., Amorin, R., Bardelli, S., Cassara, L.P., Castellano, M., Cimatti, A., Cucciati, O., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Paltani, S., Ribeiro, B., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vergani, D., Capak, P., Charlot, S., Contini, T., Cuby, J.G., Dunlop, J., Fotopoulou, S., Koekemoer, A., Lopez-Sanjuan, C., Mellier, Y., Pforr, J., Salvato, M., Scoville, N., Taniguchi, Y., Wang, P.W., Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Bologna/Università di Bologna, Université de Genève = University of Geneva (UNIGE), 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), 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
Large-scale structure of Universe, statistical [methods], Population, Dark matter, Cosmology: observations, Galaxies: evolution, Methods: statistical, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, Correlation function (astronomy), 01 natural sciences, Cosmology: observation, 0103 physical sciences, Cluster analysis, education, 010303 astronomy & astrophysics, evolution [galaxies], Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysic, observations [cosmology], Redshift, Galaxy, Amplitude, large-scale structure of Universe, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the evolution of galaxy clustering for galaxies in the redshift range 2.0, Comment: 19 pages, 10 figures, submitted to A&A

Published
2015
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114. Extreme emission-line galaxies out to z ~ 1 in zCOSMOS. I. Sample and characterization of global properties

Author

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

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Photometry (optics), Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Surface brightness, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a thorough characterization of a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 < z < 0.93 selected from the 20k zCOSMOS Bright Survey because of their unusually large emission line equivalent widths. We use multiwavelength COSMOS photometry, HST-ACS I-band imaging and optical zCOSMOS spectroscopy to derive the main global properties of EELGs, such as sizes, masses, SFRs, reliable metallicities from both "direct" and "strong-line" methods. The EELGs are compact (R_50 ~ 1.3 kpc), low-mass (log(M*/Msol)~7-10) galaxies forming stars at unusually high specific SFR (log(sSFR/yr) up to ~ -7) compared to main sequence SFGs of the same stellar mass and redshift. At UV wavelengths, the EELGs are luminous and show high surface brightness and include strong Ly$��$ emitters, as revealed by GALEX spectroscopy. We show that zCOSMOS EELGs are high-ionization, low-metallicity systems, with median 12+log(O/H)=8.16, including a handful of extremely metal-deficient galaxies (, Accepted in A&A. Final replacement to match the version in press. It includes a minor change in the title and a new figure

Published
2015

115. Reconstructing the galaxy density field with photometric redshifts: I. Methodology and validation on stellar mass functions

Author

Lucia Pozzetti, Alessandro Cimatti, Nicola Malavasi, S. Bardelli, O. Cucciati, ITA, Malavasi, N., Pozzetti, L., Cucciati, O., Bardelli, S., and Cimatti, A.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Aperture, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Measure (mathematics), 0103 physical sciences, Galaxies: distances and redshift, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, Galaxies: statistic, 010308 nuclear & particles physics, Galaxies: luminosity function, mass function, Astrophysics::Instrumentation and Methods for Astrophysics, Sigma, Astronomy and Astrophysics, Function (mathematics), Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxies: clusters: general, Methods: data analysi, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Measuring environment for large numbers of distant galaxies is still an open problem, for which we need galaxy positions and redshifts. Photometric redshifts are more easily available for large numbers of galaxies, but at the price of larger uncertainties than spectroscopic ones. In this work we study how photometric redshifts affect the measurement of galaxy environment and how this may limit an analysis of the galaxy stellar mass function (GSMF) in different environments. Using mock galaxy catalogues, we measured the environment with a fixed aperture method, using each galaxy's true and photometric redshifts. We varied the fixed aperture volume parameters and the photometric redshift uncertainties. We then computed GSMF as a function of redshift and environment. We found that only when using high-precision photometric redshifts with $\sigma_{\Delta z/(1+z)} \le 0.01$, the most extreme environments can be reconstructed in a fairly accurate way, with a fraction $\ge 60\div 80\%$ of galaxies placed in the correct density quartile and a contamination of $\le 10\%$ by opposite quartile interlopers. A volume height comparable to the $\pm 1.5\sigma$ error of photometric redshifts grants a better reconstruction than other volume configurations. When using such an environmental measure, we found that any differences between the starting GSMF (divided accordingly to the true galaxy environment) will be damped on average of $\sim 0.3$ dex when using photometric redshifts, but will be still resolvable. These results may be used to interpret real data as we obtained them in a way that is fairly independent from how well the mock catalogues reproduce the real galaxy distribution. This work represents a preparatory study for future wide area photometric redshift surveys such as the Euclid Survey and we plan to apply these results to an analysis of the GSMF in the UltraVISTA Survey in future work., Comment: Accepted for publication in Astronomy and Astrophysics

Published
2015
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116. Optically-selected clusters at 0.8 $\la$ $\mathsfsl z$ $\la$ 1.3 in the EIS cluster survey

Author

Stéphane Arnouts, L. F. Olsen, S. Bardelli, M. Scodeggio, Massimo Ramella, H. E. Jørgensen, Monique Arnaud, Andrea Biviano, E. Zucca, Doris M. Neumann, L. N. da Costa, and C. Benoist

Subjects
Physics, 010308 nuclear & particles physics, Infrared, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Redshift, Space and Planetary Science, 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

This paper presents preliminary results of a spectroscopic survey being conducted at the VLT of fields with optically-selected cluster candidates identified in the EIS I-band survey. Here we report our findings for three candidates selected for having estimated redshifts in the range z=0.8-1.1. New multi-band optical/infrared data were used to assign photometric redshifts to galaxies in the cluster fields and to select possible cluster members in preparation of the spectroscopic observations. Based on the available spectroscopic data, which includes 147 new redshifts for galaxies with Iab 99%. The detected concentrations include systems with redshifts z=0.81, z=0.95, z=1.14 and the discovery of the first optically-selected cluster at z=1.3. The latter system, with three concordant redshifts, coincides remarkably well with the location of a firm X-ray detection (>5sigma) in a ~80ksec XMM-Newton image taken as part of this program which will be presented in a future paper (Neumann et al. 2002). The z>1 systems presented here are possibly the most distant identified so far by their optical properties alone.

Published
2002
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117. The spatial clustering of X-ray selected AGN in the XMM-COSMOS field

Author

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

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

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

Published
2009
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118. Testing the radio halo-cluster merger scenario. The case of RXC J2003.5-2323

Author

E. Zucca, Rossella Cassano, Simona Giacintucci, Daniele Dallacasa, S. Bardelli, Gianfranco Brunetti, Tiziana Venturi, Pasquale Mazzotta, S. Giacintucci, T. Venturi, G. Brunetti, D. Dallacasa, P. Mazzotta, R. Cassano, S. Bardelli, and E. Zucca

Subjects
Physics, Very large array, Giant Metrewave Radio Telescope, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: clusters: individual: RXC J2003.5-2323, radiation mechanisms: non-thermal, Galaxy, Radio halo, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, galaxies: clusters: general, Cluster (physics), Halo, radiation mechanisms: non-thermal, galaxies: clusters: general, galaxies: clusters: individual: RXC J2003.5-2323, Galaxy cluster, Optical observation, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a combined radio, X-ray and optical study of the galaxy cluster RXCJ2003.5-2323. The cluster hosts one of the largest, most powerful and distant giant radio halos known to date, suggesting that it may be undergoing a strong merger process. The aim of our multiwavelength study is to investigate the radio-halo cluster merger scenario. We studied the radio properties of the giant radio halo in RXCJ2003.5-2323 by means of new radio data obtained at 1.4 GHz with the Very Large Array, and at 240 MHz with the Giant Metrewave Radio Telescope, in combination with previously published GMRT data at 610 MHz. The dynamical state of the cluster was investigated by means of X-ray Chandra observations and optical ESO--NTT observations. Our study confirms that RXCJ2003.5-2323 is an unrelaxed cluster. The unusual filamentary and clumpy morphology of the radio halo could be due to a combination of the filamentary structure of the magnetic field and turbulence in the inital stage of a cluster merger., 10 page, 10 figures, accepted for publication on A&A

Published
2009

119. Hidden starbursts and active galactic nuclei at 0< z <4 from the Herschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Author

Roy R. Gal, E. Zucca, Dale D. Kocevski, G. Zamorani, Olivier Ilbert, Brian C. Lemaux, Olivier Le Fevre, Lori M. Lubin, Paolo Cassata, Paolo Ciliegi, Gordon K. Squires, Emeric Le Floc'h, Laurence Tresse, Elizabeth J. McGrath, 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire AIM, and Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay

Subjects
submillimeter: galaxies, Active galactic nucleus, Field (physics), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], galaxies: active, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: high-redshift, Astrophysics::Solar and Stellar Astrophysics, Coevolution, Astrophysics::Galaxy Astrophysics, Physics, Galaxies: active, Galaxies: evolution, Galaxies: high-redshift, Galaxies: starburst, Submillimeter: galaxies, Techniques: spectroscopic, Astronomy and Astrophysics, Space and Planetary Science, Conjunction (astronomy), Galaxy, Redshift, Spire, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cosmic time, techniques: spectroscopic, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate of the properties of $\sim$2000 Herschel/SPIRE-selected galaxies from $00.5$), the highest $L_{TIR}$ galaxies in a given redshift bin are unobserved by SPIRE at subsequently lower redshifts, a trend linked to downsizing. In conjunction with other results, this evidence is used to argue for prevalent AGN-driven quenching in starburst galaxies across cosmic time., Comment: 39 pages, 19 figures, 6 tables, accepted to A&A. Updated version contains minor revisions and corrects a typo made in equation 5. All data used in the paper is now available online through CDS

Published
2014
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120. Discovery of a rich proto-cluster at z = 2.9 and associated diffuse cold gas in the VIMOS Ultra-Deep Survey (VUDS)

Author

Letizia P. Cassarà, Alessandro Cimatti, C. Moreau, Mara Salvato, V. Le Brun, Paolo Cassata, Margherita Talia, Nimish P. Hathi, O. Le Fèvre, Laurence Tresse, S. de la Torre, S. Bardelli, A. Durkalec, Sotiria Fotopoulou, C. López-Sanjuan, Adriano Fontana, P. W. Wang, Yoshiaki Taniguchi, Eros Vanzella, R. Thomas, Thierry Contini, M. Giavalisco, Peter Capak, Stephane Charlot, E. Zucca, Andrea Grazian, B. Ribeiro, G. Zamorani, Olga Cucciati, Yannick Mellier, D. Maccagni, Stéphane Paltani, Marco Castellano, M. Scodeggio, Olivier Ilbert, Ricardo Amorín, Laura Pentericci, N. Z. Scoville, Bianca Garilli, Daniela Vergani, Jean-Gabriel Cuby, Brian C. Lemaux, V. Sommariva, Lidia Tasca, Daniel Schaerer, 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), Cucciati, O., Zamorani, G., Lemaux, B.C., Bardelli, S., Cimatti, A., Le Fèvre, O., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Tasca, L.A.M., Thomas, R., Vanzella, E., Zucca, E., Amorin, R., Capak, P., Cassarà, L.P., Castellano, M., Cuby, J.G., De La Torre, S., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.W., Charlot, S., Contini, T., Fotopoulou, S., López-Sanjuan, C., Mellier, Y., Scoville, N., and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Line-of-sight, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Radio galaxy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Rest frame, Astronomy and Astrophysic, Cosmology: observations, Galaxies: high-redshift, Large-scale structure of Universe, Space and Planetary Science, Cosmology: observation, Redshift, Galaxy, galaxies: high-redshift, cosmology: observations, Galaxy formation and evolution, [INFO]Computer Science [cs], Halo, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

[Abridged] We characterise a massive proto-cluster at z=2.895 that we found in the COSMOS field using the spectroscopic sample of the VIMOS Ultra-Deep Survey (VUDS). This is one of the rare structures at z~3 not identified around AGNs or radio galaxies, so it is an ideal laboratory to study galaxy formation in dense environments. The structure comprises 12 galaxies with secure spectroscopic redshift in an area of 7'x8', in a z bin of Dz=0.016. The measured galaxy number overdensity is delta_g=12+/-2. This overdensity has total mass of M~8.1x10^(14)M_sun in a volume of 13x15x17 Mpc^3. Simulations indicate that such an overdensity at z~2.9 is a proto-cluster that will collapse in a cluster of total mass M~2.5x10^(15)M_sun at z=0. We compare the properties of the galaxies within the overdensity with a control sample at the same z but outside the overdensity. We did not find any statistically significant difference between the properties (stellar mass, SFR, sSFR, NUV-r, r-K) of the galaxies inside and outside the overdensity. The stacked spectrum of galaxies in the overdensity background shows a significant absorption feature at the wavelength of Lya redshifted at z=2.895 (lambda=4736 A), with a rest frame EW = 4+/- 1.4 A. Stacking only background galaxies without intervening sources at z~2.9 along their line of sight, we find that this absorption feature has a rest frame EW of 10.8+/-3.7 A, with a detection S/N of ~4. These EW values imply a high column density (N(HI)~3-20x10^(19)cm^(-2)), consistent with a scenario where such absorption is due to intervening cold gas streams, falling into the halo potential wells of the proto-cluster galaxies. However, we cannot exclude the hypothesis that this absorption is due to the diffuse gas within the overdensity., Comment: 15 pages, 9 figures, accepted for publication in A&A (revised version after referee's comments and language editing)

Published
2014
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121. MOLECULAR GAS IN THE X-RAY BRIGHT GROUP NGC 5044 AS REVEALED BY ALMA

Author

Youichi Ohyama, Christine Jones, Philippe Salomé, Jeremy Lim, Simona Giacintucci, Fabrizio Brighenti, Francoise Combes, Ming Sun, Ewan O'Sullivan, Fabio Gastaldello, Stephen Hamer, Jan M. Vrtilek, Laurence P. David, Henrique R. Schmitt, William R. Forman, Alastair C. Edge, Pasquale Temi, Dinh-V Trung, William G. Mathews, S. Bardelli, Littoral, Environnement, Télédétection, Géomatique (LETG - Brest), Littoral, Environnement, Télédétection, Géomatique UMR 6554 (LETG), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-Université d'Angers (UA)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Brest (UBO)-Université de Rennes 2 (UR2), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Géographie et d'Aménagement Régional de l'Université de Nantes (IGARUN), Université de Nantes (UN)-Université de Nantes (UN)-Université de Caen Normandie (UNICAEN), Université de Nantes (UN)-Université de Nantes (UN), 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut de Chimie de la Matière Condensée de Bordeaux (ICMCB), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut Polytechnique de Bordeaux-Université de Bordeaux (UB), University of California [San Diego] (UC San Diego), University of California, Normandie Université (NU)-Normandie Université (NU)-Université d'Angers (UA)-École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Brest (UBO)-Université de Rennes 2 (UR2)-Centre National de la Recherche Scientifique (CNRS)-Institut de Géographie et d'Aménagement Régional de l'Université de Nantes (IGARUN), École normale supérieure - Paris (ENS-PSL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California (UC), Laurence P. David, Jeremy Lim, William Forman, Jan Vrtilek, Francoise Combe, Philippe Salome, Alastair Edge, Stephen Hamer, Christine Jone, Ming Sun, Ewan O'Sullivan, Fabio Gastaldello, Sandro Bardelli, Pasquale Temi, Henrique Schmitt, Youichi Ohyama, William Mathew, Fabrizio Brighenti, Simona Giacintucci, and Dinh-V Trung

Subjects
active [Galaxies], astro-ph.GA, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], Cooling flow, Laser linewidth, galaxies: groups: individual: NGC 5044, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], Supermassive black hole, Molecular cloud, Spatially resolved, groups: individual (NGC 5044) [Galaxies], X-ray, Velocity dispersion, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, ISM. [Galaxies], galaxies: clusters: general, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract

A short 30 minute ALMA observation of the early-type galaxy NGC 5044, which resides at the center of an X-ray bright group with a moderate cooling flow, has detected 24 molecular structures within the central 2.5 kpc. The masses of the molecular structures vary from 3e5 to 1e7 Mo3 and the CO(2-1) linewidths vary from 15 to 65 km/s. Given the large CO(2-1) linewidths, the observed structures are likely giant molecular associations (GMAs) and not individual molecular clouds (GMCs). Only a few of the GMAs are spatially resolved with the cycle 0 ALMA beam and the average density of these GMAs yields a GMC volume filling factor of about 15%. The observed masses of the resolved GMAs are insufficient for them to be gravitationally bound, however, the most massive GMA does contain a less massive component with a linewidth of 5.5 km/s (typical of an individual virialized GMC). We also show that the GMAs cannot be pressure confined by the hot gas. Given the observed CO(2-1) linewidths of the GMAs (i.e., the velocity dispersion of the embedded GMCs) they will likely disperse on a timescale of about 12 Myr, which is less than the central cooling time of the hot gas, so the embedded GMCs within a GMA must condense out of the hot gas at the same time and arise from local concentrations of thermally unstable parcels of hot gas. There are no indications of any disk-like molecular structures and all indications suggest that the molecular gas follows ballistic trajectories after condensing out of the thermally unstable hot gas. The 230 GHz luminosity of the central continuum source is 500 times greater than its low frequency radio luminosity and probably reflects a recent accretion event by the central supermassive black hole. The spectrum of the central continuum source also exhibits an absorption feature.

Published
2014
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123. The zCOSMOS redshift survey : evolution of the light in bulges and discs since z ~ 0.8

Author

Luis C. Ho, O. Le Fevre, H. J. McCracken, P. Franzetti, Anton M. Koekemoer, R. Pello, E. Zucca, A. Cappi, A. Cattaneo, Niraj Welikala, A. Iovino, K. Kovavc, Alvio Renzini, J. F. Le Borgne, R. M. Rich, M. Mignoli, B. Garilli, T. Contini, Yoshiaki Taniguchi, Graziano Coppa, Jean-Paul Kneib, Masaomi Tanaka, C. Lopez-Sanjuan, E. Perez Montero, P. Kampczyk, Vincenzo Mainieri, Andrea Cimatti, F. Lamareille, Richard Massey, Marco Scodeggio, Angela Bongiorno, Rongmon Bordoloi, Y. Peng, L. Tresse, L. A. M. Tasca, C. Knobel, S. Bardelli, Duncan Farrah, Kartik Sheth, Christian Maier, D. Vergani, Michele Moresco, O. Cucciati, S. de la Torre, K. Caputi, C. M. Carollo, M. Bolzonella, Lucia Pozzetti, G. Zamorani, C. T. Liu, D. B. Sanders, Simon J. Lilly, Luigi Guzzo, V. Le Brun, O. Ilbert, Astronomy, Tasca, L.A.M., Tresse, L., Le Fèvre, O., Ilbert, O., Lilly, S.J., Zamorani, G., López-Sanjuan, C., Ho, L.C., Bardelli, S., Cattaneo, A., Cucciati, O., Farrah, D., Iovino, A., Koekemoer, A.M., Liu, C.T., Massey, R., Renzini, A., Taniguchi, Y., Welikala, N., Zucca, E., Carollo, C.M., Contini, T., Kneib, J.-P., Mainieri, V., Scodeggio, M., Bolzonella, M., Bongiorno, A., Caputi, K., De La Torre, S., Franzetti, P., Garilli, B., Guzzo, L., Kampczyk, P., Knobel, C., Kovač, K., Lamareille, F., Le Borgne, J.-F., Le Brun, V., Maier, C., Mignoli, M., Pello, R., Peng, Y., Perez Montero, E., Rich, R.M., Tanaka, M., Vergani, D., Bordoloi, R., Cappi, A., Cimatti, A., Coppa, G., Mccracken, H.J., Moresco, M., Pozzetti, L., Sanders, D., and Sheth, K.

Subjects
Galaxies: fundamental parameter, FORMING GALAXY, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, fundamental parameters. [Galaxies], LUMINOSITY FUNCTIONS, galaxies: bulges, STAR-FORMATION RATE, Luminosity, ADVANCED CAMERA, bulges [Galaxies], Bulge, distances and redshifts [Galaxies], Galaxies: distances and redshift, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Physics, FORMATION HISTORY, Star formation, Astronomy and Astrophysics, galaxies: fundamental parameters, HUBBLE-SPACE-TELESCOPE, VLT DEEP SURVEY, Astronomy and Astrophysic, Redshift survey, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, luminosity function [Galaxies], Redshift, Galaxy, Stars, galaxies: luminosity function, Space and Planetary Science, mass function, Astrophysics of Galaxies (astro-ph.GA), galaxies: luminosity function, mass function, Astrophysics::Earth and Planetary Astrophysics, GALAXY FORMATION, galaxies: distances and redshifts, Irregular galaxy, galaxies: evolution, Galaxies: bulge, SURVEY COSMOS
Abstract

We studied the chronology of galactic bulge and disc formation by analysing the relative contributions of these components to the B-band rest-frame luminosity density at different epochs. We present the first estimate of the evolution of the fraction of rest-frame B-band light in galactic bulges and discs since redshift z~0.8. We performed a bulge-to-disc decomposition of HST/ACS images of 3266 galaxies in the zCOSMOS-bright survey with spectroscopic redshifts in the range 0.7 < z < 0.9. We find that the fraction of B-band light in bulges and discs is $(26 \pm 4)%$ and $(74 \pm 4)%$, respectively. When compared with rest-frame B-band measurements of galaxies in the local Universe in the same mass range ($10^{9} M_{\odot}\lessapprox M \lessapprox 10^{11.5} M_{\odot}$), we find that the B-band light in discs decreases by ~30% from z~0.7-0.9 to z~0, while the light from the bulge increases by ~30% over the same period of time. We interpret this evolution as the consequence of star formation and mass assembly processes, as well as morphological transformation, which gradually shift stars formed at half the age of the Universe from star-forming late-type/irregular galaxies toearlier types and ultimately into spheroids., Letter to the Editor, 4 pages, 2 figures, accepted for publication in Astronomy and Astrophysics

Published
2014

124. Discovering extremely compact and metal-poor, star-forming dwarf galaxies out to z ~ 0.9 in the VIMOS Ultra-Deep Survey

Author

D. Maccagni, C. López-Sanjuan, Stéphane Paltani, Yoshiaki Taniguchi, Eros Vanzella, Daniela Vergani, Andrea Grazian, O. Le Fèvre, Thierry Contini, Ricardo Amorín, Margherita Talia, M. Giavalisco, Nimish P. Hathi, Peter Capak, G. Zamorani, S. Bardelli, V. Le Brun, Rajat M. Thomas, E. Zucca, Sotiria Fotopoulou, Letizia P. Cassarà, S. de la Torre, P. Cassata, M. Scodeggio, Brian C. Lemaux, N. Z. Scoville, Jean-Gabriel Cuby, Alessandro Cimatti, Bianca Garilli, Adriano Fontana, Laura Pentericci, Laurence Tresse, Mara Salvato, P. W. Wang, B. Ribeiro, Lidia Tasca, A. Durkalec, C. Moreau, V. Sommariva, Daniel Schaerer, Yannick Mellier, Olga Cucciati, Stephane Charlot, Marco Castellano, Olivier Ilbert, Amorín, R., Sommariva, V., Castellano, M., Grazian, A., Tasca, L.A.M., Fontana, A., Pentericci, L., Cassata, P., Garilli, B., Le Brun, V., Le Fèvre, O., Maccagni, D., Thomas, R., Vanzella, E., Zamorani, G., Zucca, E., Bardelli, S., Capak, P., Cassará, L.P., Cimatti, A., Cuby, J.G., Cucciati, O., De La Torre, S., Durkalec, A., Giavalisco, M., Hathi, N.P., Ilbert, O., Lemaux, B.C., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.W., Charlot, S., Contini, T., Fotopoulou, S., López-Sanjuan, C., Mellier, Y., Scoville, N., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), European Project: 312725,EC:FP7:SPA,FP7-SPACE-2012-1,ASTRODEEP(2013), 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), 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
Galaxies: fundamental parameters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Galaxies: abundances, Galaxies: fundamental parameter, FOS: Physical sciences, Astrophysics, Photometry (optics), Ionization, Galaxies: dwarf, Galaxies: evolution, Galaxies: high-redshift, Galaxies: starburst, Astronomy and Astrophysics, Space and Planetary Science, [INFO]Computer Science [cs], Emission spectrum, Dwarf galaxy, Physics, Star formation, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: abundance, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the discovery of 31 low-luminosity (-14.5 > M_{AB}(B) > -18.8), extreme emission line galaxies (EELGs) at 0.2 < z < 0.9 identified by their unusually high rest-frame equivalent widths (100 < EW[OIII] < 1700 A) as part of the VIMOS Ultra Deep Survey (VUDS). VIMOS optical spectra of unprecedented sensitivity ($I_{AB}$ ~ 25 mag) along with multiwavelength photometry and HST imaging are used to investigate spectrophotometric properties of this unique sample and explore, for the first time, the very low stellar mass end (M* < 10^8 M$_{\odot}$) of the luminosity-metallicity (LZR) and mass-metallicity (MZR) relations at z < 1. Characterized by their extreme compactness (R50 < 1 kpc), low stellar mass and enhanced specific star formation rates (SFR/M* ~ 10^{-9} - 10^{-7} yr^{-1}), the VUDS EELGs are blue dwarf galaxies likely experiencing the first stages of a vigorous galaxy-wide starburst. Using T_e-sensitive direct and strong-line methods, we find that VUDS EELGs are low-metallicity (7.5 < 12+log(O/H) < 8.3) galaxies with high ionization conditions, including at least three EELGs showing HeII 4686A emission and four EELGs of extremely metal-poor (, Letter in A&A 568, L8 (2014). This replacement matches the published version

Published
2014
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125. Shock acceleration as origin of the radio relic in A521?

Author

G. Brunetti, S. Bardelli, G. Macario, Tiziana Venturi, Maxim Markevitch, Daniele Dallacasa, R. Athreya, Simona Giacintucci, Rossella Cassano, S. Giacintucci, T. Venturi, G. Macario, D. Dallacasa, G. Brunetti, M. Markevitch, R. Cassano, S. Bardelli, and R. Athreya

Subjects
Physics, Spectral index, Giant Metrewave Radio Telescope, GALAXIES: CLUSTERS: INDIVIDUAL: A 521, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio spectrum, Shock (mechanics), Radio relics, GALAXIES: CLUSTERS: GENERAL, Radio halo, Space and Planetary Science, Intracluster medium, RADIO CONTINUUM: GALAXIES, Surface brightness, Astrophysics::Galaxy Astrophysics
Abstract

We present new high sensitivity observations of the radio relic in A521 carried out with the Giant Metrewave Radio Telescope at 327 MHz and with the Very Large Array at 4.9 and 8.5 GHz. We imaged the relic at these frequencies and carried out a detailed spectral analysis, based on the integrated radio spectrum between 235 MHz and 4.9 GHz, and on the spectral index image in the frequency range 327-610 MHz. To this aim we used the new GMRT observations and other proprietary as well as archival data. We also searched for a possible shock front co-located with the relic on a short archival Chandra X-ray observation of the cluster. The integrated spectrum of the relic is consistent with a single power law; the spectral index image shows a clear trend of steepening going from the outer portion of the relic toward the cluster centre. We discuss the origin of the source in the light of the theoretical models for the formation of cluster radio relics. Our results on the spectral properties of the relic are consistent with acceleration of relativistic electrons by a shock in the intracluster medium. This scenario is further supported by our finding of an X-ray surface brightness edge coincident with the outer border of the radio relic. This edge is likely a shock front., 13 pages, 12 figures, accepted for publication in A&A

Published
2008

126. Revised statistics of radio halos and the reacceleration model

Author

Simona Giacintucci, G. Brunetti, Rossella Cassano, S. Bardelli, Tiziana Venturi, Daniele Dallacasa, Giancarlo Setti, R. Cassano, G. Brunetti, T. Venturi, G. Setti, D. Dallacasa, S. Giacintucci, and S. Bardelli

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, RADIO CONTINUUM: GENERAL, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, RADIATION MECHANISM: NON-THERMAL, FOS: Physical sciences, Astronomy and Astrophysics, LOFAR, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift, Luminosity, X-RAYS: GENERAL, Radio halo, GALAXIES: CLUSTERS: GENERAL, Space and Planetary Science, Range (statistics), Cluster (physics), Halo, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

Aims. The statistical properties of radio halos can be used to discriminate among the possible models for their origin. Therefore an unbiased and exhaustive investigation in this direction is crucial. Methods. With this goal in mind in this paper we revise the occurrence of radio halos in the redshift range 0-0.4, combining the low redshift (z, Comment: 12 pages, 10 figures. Accepted by A&A

Published
2008

127. GMRT Radio Halo Survey in galaxy clusters at z = 0.2 -- 0.4. II.The eBCS clusters and analysis of the complete sample

Author

S. Bardelli, Tiziana Venturi, Simona Giacintucci, Daniele Dallacasa, Giancarlo Setti, Gianfranco Brunetti, Rossella Cassano, T. Venturi, S. Giacintucci, D. Dallacasa, R. Cassano, G. Brunetti, S. Bardelli, and G. Setti

Subjects
Physics, Giant Metrewave Radio Telescope, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Sample (graphics), Redshift, Radio halo, GALAXIES: CLUSTERS: GENERAL, Space and Planetary Science, Primary (astronomy), Cluster (physics), RADIO CONTINUUM: GALAXIES, Halo, Galaxy cluster, Astrophysics::Galaxy Astrophysics
Abstract

We present the results of the GMRT cluster radio halo survey. The main purposes of our observational project are to measure which fraction of massive galaxy clusters in the redshift range z=0.2--0.4 hosts a radio halo, and to constrain the expectations of the particle re--acceleration model for the origin of the non--thermal radio emission. We selected a complete sample of 50 clusters in the X-ray band from the REFLEX (27) and the eBCS (23) catalogues. In this paper we present Giant Metrewave Radio Telescope (GMRT) observations at 610 MHz for all clusters still lacking high sensitivity radio information, i.e. 16 eBCS and 7 REFLEX clusters, thus completing the radio information for the whole sample. The typical sensitivity in our images is in the range 1$\sigma \sim 35-100 \mu$Jy b$^{-1}$. We found a radio halo in A697, a diffuse peripheral source of unclear nature in A781, a core--halo source in Z7160, a candidate radio halo in A1682 and ``suspect'' central emission in Z2661. Including the literature information, a total of 10 clusters in the sample host a radio halo. A very important result of our work is that 25 out of the 34 clusters observed with the GMRT do not host extended central emission at the sensitivity level of our observations, and for 20 of them firm upper limits to the radio power of a giant radio halo were derived. The GMRT Radio Halo Survey shows that radio halos are not common, and our findings on the fraction of giant radio halos in massive clusters are consistent with the statistical expectations based on the re--acceleration model. Our results favour primary to secondary electron models., Comment: A&A in press, 17 pages, 12 figures, 4 tables Version with high quality figures available on web at http://www.ira.inaf.it/~tventuri/pap/Venturi_web.pdf

Published
2008
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128. Radio properties of the Shapley Concentration -- III. Merging clusters in the A3558 complex

Author

Raffaella Morganti, Richard W. Hunstead, S. Bardelli, and Tiziana Venturi

Subjects
NRAO VLA Sky Survey, Physics, Radio galaxy, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, Radio halo, Space and Planetary Science, Cluster (physics), Halo, Source counts, Luminosity function (astronomy)
Abstract

We present the results of a 22 cm radio survey carried out with the A3558 complex, a chain formed by the merging ACO clusters A3556-A3558-A3562 and thetwo groups SC1327-312 and SC1323-313, located in the central region of the complex, a chain formed by the merging ACO clusters A3556-A3558-A3562 and the two groups SC1327-312 and SC1323-313, located in the central region of the Shapley Concentration. The purpose of our survey is to study the effects of cluster mergers on the statistical properties of radio galaxies and to investigate the connection between mergers and the presence of radio halos and relic sources. We found that the radio source counts in the A3558 complex are consistent with the background source counts. Furthermore, we found that no correlation exists between the local density and the radio source power, and that steep spectrum radio galaxies are not segregated in denser optical regions. The radio luminosity function for elliptical and S0 galaxies is significantly lower than that for cluster type galaxies and for those not selected to be in clusters at radio powers logP(1.4) > 22.5, implying that the probability of a galaxy becoming a radio source above this power limit is lower in the Shapley Concentration compared with any other environment. The detection of a head-tail source in the centre of A3562, coupled with careful inspection of the 20 cm NRAO VLA Sky Survey (NVSS) and of 36 cm MOST observations, allowed us to spot two extended sources in the region between A3562 and SC1329-313, i.e. a candidate radio halo at the centre of A3562, and low brightness extended emission around a 14.96 magnitude Shapley galaxy., 18 pages, 14 figures. Accepted for publication on MNRAS

Published
2000
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129. The VIMOS-VLT Deep Survey: Mass and light clustering in the Universe during the last 8 billion years

Author

A. Pollo, U. Abbas, B. Meneux, L. Guzzo, O. . Fevre, A. Cappi, H. J. McCracken, A. Iovino, C. Marinoni, D. Bottini, B. Garilli, V. . 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, P. Franzetti, I. Gavignaud, O. Ilbert, B. Marano, A. Mazure, R. Merighi, S. Paltani, R. Pello, L. Pozzetti, M. Radovich, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, S. . La, F. Lamareille, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, C. J. Walcher, CUCCIATI, OLGA, A. Pollo, U. Abba, B. Meneux, L. Guzzo, O. . Fevre, A. Cappi, H. J. McCracken, A. Iovino, C. Marinoni, D. Bottini, B. Garilli, V. . Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnout, S. Bardelli, M. Bolzonella, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, O. Ilbert, B. Marano, A. Mazure, R. Merighi, S. Paltani, R. Pello, L. Pozzetti, M. Radovich, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, O. Cucciati, S. . La, F. Lamareille, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, and C. J. Walcher

Subjects
pancake, cosmological constant, Observational cosmology (including Hubble constant, Superclusters, large-scale structure of the Universe (including void, great wall, etc.), Astrophysics::Cosmology and Extragalactic Astrophysics, early Universe, distance scale, Astrophysics::Galaxy Astrophysics
Abstract

Using the first-epoch data from the VIMOS-VLT Deep Survey (VVDS), we investigate the evolution of the projected two-point correlation function of galaxies between z ∼ 1 and the present epoch. For the global galaxy population we do not find strong variations of clustering with redshift. However, dependence of clustering on intrinsic luminosities and stellar masses of galaxies evolves significantly during this period. We observe more close pairs for the most luminous and (less distinctly) most massive objects at z ∼ 1 as compared to what is seen locally, resulting in a non–power-law shape of their correlation function, with an upturn on small scales. This effect can be modeled within the framework of the halo occupation distribution models and leads to the conclusion that at z ∼ 1 we are possibly observing a population of luminous and not very massive satellite galaxies that occupy the most massive dark-matter halos—an effect that is not seen locally.

Published
2007

130. The VIMOS VLT Deep Survey: Star Formation Since z~5 and Mass Assembly from the VVDS-SWIRE Sample

Author

O. . Fevre, S. Arnouts, L. Tresse, O. Ilbert, C. Lonsdale, M. Polletta, M. Rowan Robinson, G. Zamorani, E. Zucca, S. Bardelli, S. Paltani, L. Pozzetti, D. Bottini, B. Garilli, V. . Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, D. Shupe, J. Surace, G. Vettolani, A. Zanichelli, C. Adami, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, A. Iovino, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, R. Pello, A. Pollo, M. Radovich, M. Bondi, A. Bongiorno, J. Brinchmann, S. . La, F. Lamareille, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, C. J. Walcher, CUCCIATI, OLGA, O. . Fevre, S. Arnout, L. Tresse, O. Ilbert, C. Lonsdale, M. Polletta, M. Rowan-Robinson, G. Zamorani, E. Zucca, S. Bardelli, S. Paltani, L. Pozzetti, D. Bottini, B. Garilli, V. . Brun, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, D. Shupe, J. Surace, G. Vettolani, A. Zanichelli, C. Adami, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, O. Cucciati, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, A. Iovino, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, R. Pello, A. Pollo, M. Radovich, M. Bondi, A. Bongiorno, J. Brinchmann, S. . La, F. Lamareille, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, and C. J. Walcher

Subjects
GALAXY LUMINOSITY FUNCTION, 1ST EPOCH DATA, EVOLUTION, HISTORY, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The VIMOS VLT Deep Survey is enabling to trace from one single survey the star formation history in the Universe over 12 billion years of evolution. We find that the star formation rate is strongly linked to the different types of galaxies. While the Luminosity Density of irregular-like galaxies decreased by more than a factor 3.5 from z = 1.2 to z = 0.2, the LD for early-type galaxies increased by a factor 1.7. Star formation happened in several phases, strongly luminosity dependent, with star formation gradually shifting from the first massive galaxies to less massive systems. The peak in SFR at z = 3.5 is identified with the end of the mass assembly of the most luminous galaxies (M-AB(1500 angstrom) < -21). We use the SWIRE Spitzer-IRAC observations of the VVDS-02h field to assemble a flux-limited sample at 3.8 mu m of 1500 galaxies with spectroscopic redshifts and more than 22000 galaxies with photometric redshifts up to z = 2 and build the rest-frame K-band luminosity function and stellar mass density. We find that the global stellar mass density has remained relatively constant since z similar to 1, but the epoch 1 < z < 2 has seen an increase of more than a factor 10 in the stellar mass density of red galaxies selected based on the bimodal distribution of (NUV-r) colors, while in the same period blue galaxies have seen only a modest factor 2 increase. We interpret this as the fast build-up of the red sequence of galaxies, essentially complete by z similar to 1.

Published
2007

131. Highlights from the VIMOS VLT Deep Survey

Author

O. . Fevre, B. Garilli, V. . Brun, D. Maccagni, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, D. Bottini, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, O. Ilbert, A. Iovino, F. Lamareille, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, S. Paltani, R. Pello, A. Pollo, L. Pozzetti, M. Radovich, D. Vergani, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, S. . La, L. . Ravel, L. Gregorini, E. Perez Montero, Y. Mellier, P. Merluzzi, S. Temporin, C. J. Walcher, CUCCIATI, OLGA, O. . Fevre, B. Garilli, V. . Brun, D. Maccagni, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnout, S. Bardelli, M. Bolzonella, D. Bottini, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, O. Ilbert, A. Iovino, F. Lamareille, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, S. Paltani, R. Pello, A. Pollo, L. Pozzetti, M. Radovich, D. Vergani, G. Zamorani, E. Zucca, M. Bondi, A. Bongiorno, J. Brinchmann, O. Cucciati, S. . La, L. . Ravel, L. Gregorini, E. Perez-Montero, Y. Mellier, P. Merluzzi, S. Temporin, and C. J. Walcher

Subjects
Galaxy group, cluster, Characteristics and properties of external galaxies and extragalactic objects, and superclusters, large scale structure of the Universe
Abstract

Taking advantage of the efficient VIMOS multi-slit spectrograph on the VLT, we are conducting the VIMOS VLT Deep Survey (VVDS), aimed to trace the evolution of galaxies and large-scale structures over more than 90% of the life of the Universe. The VVDS is made of three magnitude selected surveys: the wide survey at IAB = 22.5, the deep survey at IAB = 24, and the ultra-deep survey at IAB = 24.75. To date, the VVDS has assembled more than 45000 redshifts in the range 0 < z ≤ 5. A number of results have been obtained, including a comprehensive view of the luminosity and stellar mass evolution as a function of galaxy type over 0 < z ≤ 2, a detailed look at the evolution of the clustering of galaxies as a function of type and environment, and a complete census of the actively star-forming galaxy population for 1.5 < z ≤ 5. This paper focuses on current highlights and on-going work from the VVDS.

Published
2007

132. 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

133. The VVDS type-1 AGN sample: the faint end of the luminosity function

Author

A. Bongiorno, G. Zamorani, I. Gavignaud, B. Marano, S. Paltani, G. Mathez, P. Møller, J. P. Picat, M. Cirasuolo, F. Lamareille, D. Bottini, B. Garilli, V. Le Brun, O. Le Fèvre, D. Maccagni, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, L. Guzzo, O. Ilbert, A. Iovino, H. J. McCracken, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, R. Pellò, A. Pollo, L. Pozzetti, M. Radovich, E. Zucca, E. Hatziminaoglou, M. Polletta, M. Bondi, J. Brinchmann, O. Cucciati, S. de la Torre, L. Gregorini, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, C. J. Walcher, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), INAF-Osservatorio Astronomico di Bologna (OABO), Astrophysikalisches Institut Potsdam (AIP), INTEGRAL Science Data Centre, 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), European Southern Observatory (ESO), University of Edinburgh, 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), IRA-INAF, Bologna, 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, INAF-Osservatorio Astronomico di Brera, Institute for Astronomy, University of Hawaii, 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), Astronomical Observatory, Jagiellonia University, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Center for Astrophysics and Space Sciences, University of California, San Diego, Centro de Astrofisica da Universidade do Porto (CAUP), AUTRES, 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), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), 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), 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), 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), A. Bongiorno, G. Zamorani, I. Gavignaud, B. Marano, S. Paltani, G. Mathez, J.P. Picat, M. Cirasuolo, F. Lamareille, D. Bottini, B. Garilli, V. Le Brun, O. Le Fevre, D. Maccagni, R. Scaramella, M. Scodeggio, L. Tresse, G. Vettolani, A. Zanichelli, C. Adami, S. Arnout, S. Bardelli, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, L. Guzzo, O. Ilbert, A. Iovino, H.J. McCracken, C. Marinon, A. Mazure, B. Meneux, R. Merighi, R. Pello', A. Pollo, L. Pozzetti, M. Radovich, E. Zucca, E. Hatziminaoglou, M. Polletta, M. Bondi, J. Brinchmann, O. Cucciati, S. de la Torre, L. Gregorini, Y. Mellier, P. Merluzzi, S. Temporin, D. Vergani, and C.J. Walcher

Subjects
Physics, Active galactic nucleus, COSMIC cancer database, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Redshift, Luminosity, [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), Range (statistics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract

In a previous paper (Gavignaud et al. 2006), we presented the type-1 Active Galactic Nuclei (AGN) sample obtained from the first epoch data of the VIMOS-VLT Deep Survey (VVDS). The sample consists of 130 faint, broad-line AGN with redshift up to z=5 and 17.5< I, 13 pages, 10 figures, submitted to A&A

Published
2007
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134. 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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136. VIMOS Ultra-Deep Survey (VUDS): Witnessing the Assembly of a Massive Cluster at z~3.3

Author

R. Thomas, Andrea Grazian, Jean-Gabriel Cuby, Daniel Schaerer, S. de la Torre, E. Zucca, Laurence Tresse, Letizia P. Cassarà, Dale D. Kocevski, Marco Castellano, Olivier Ilbert, D. Maccagni, N. Z. Scoville, Ricardo Amorín, Andrea Cimatti, T. Sadibekova, Stéphane Paltani, V. Sommariva, Sotiria Fotopoulou, Lidia Tasca, Stephane Charlot, Thierry Contini, C. López-Sanjuan, A. Durkalec, Margherita Talia, Yannick Mellier, Bianca Garilli, G. Zamorani, S. Bardelli, Olga Cucciati, L. M. Lubin, Daniela Vergani, Adriano Fontana, M. Scodeggio, B. Ribeiro, M. Giavalisco, P. W. Wang, Laura Pentericci, Peter Capak, Nimish P. Hathi, Brian C. Lemaux, V. Le Brun, Paolo Cassata, Yoshiaki Taniguchi, Eros Vanzella, C. Moreau, O. Le Fèvre, Roy R. Gal, Mara Salvato, 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Lemaux, B.C., Cucciati, O., Tasca, L.A.M., Le Fèvre, O., Zamorani, G., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Amorín, R., Bardelli, S., Capak, P., Cassarà, L.P., Castellano, M., Cimatti, A., Cuby, J.G., De La Torre, S., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Moreau, C., Paltani, S., Ribeiro, B., Salvato, M., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Taniguchi, Y., Tresse, L., Vergani, D., Wang, P.W., Charlot, S., Contini, T., Fotopoulou, S., Gal, R.R., Kocevski, D.D., López-Sanjuan, C., Lubin, L.M., Mellier, Y., Sadibekova, T., and Scoville, N.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, galaxies: active, FOS: Physical sciences, Astrophysics, Spectral line, techniques: photometric, galaxies: high-redshift, Coma Cluster, Galaxies: active, Galaxies: clusters: general, Galaxies: evolution, Galaxies: high-redshift, Techniques: photometric, Techniques: spectroscopic, Astronomy and Astrophysics, Space and Planetary Science, Photometric redshift, media_common, Physics, Star formation, Astronomy and Astrophysic, Redshift, Galaxy, Universe, galaxies: clusters: general, Halo, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using new spectroscopic observations obtained as part of the VIMOS Ultra-Deep Survey (VUDS), we perform a systematic search for overdense environments in the early universe ($z>2$) and report here on the discovery of Cl J0227-0421, a massive protocluster at $z=3.29$. This protocluster is characterized by both the large overdensity of spectroscopically confirmed members, $\delta_{gal}=10.5\pm2.8$, and a significant overdensity in photometric redshift members. The halo mass of this protocluster is estimated, by a variety of methods, to be roughly $3\times10^{14}$ $\mathcal{M}_{\odot}$ at $z\sim3.3$, which, evolved to $z=0$ results in a halo mass rivaling or exceeding that of the Coma cluster. The properties of 19 spectroscopically confirmed member galaxies are compared with a large sample of VUDS/VVDS galaxies in lower density field environments at similar redshifts. We find tentative evidence for an excess of redder, brighter, and more massive galaxies within the confines of the protocluster relative to the field population, which suggests that we may be observing the beginning of environmentally-induced quenching. The properties of these galaxies are investigated, including a discussion of the brightest protocluster galaxy which appears to be undergoing vigorous coeval nuclear and starburst activity. The remaining member galaxies appear to have characteristics which are largely similar to the field population. Though we find weaker evidence of the suppression of the median star formation rates amongst and differences in stacked spectra of member galaxies with respect to the field, we defer any conclusions of these trends to future work with the ensemble of protostructures that are found in the full VUDS sample., Comment: 23 pages, 15 figures, 3 tables, accepted for publication in A&A after minor changes, v3/v4 contains an additional online table and minor topical changes

Published
2014
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137. Evidence for major mergers of galaxies at 2 ≲ z < 4 in the VVDS and VUDS surveys

Author

L. A. M. Tasca, O. Le Fèvre, C. López-Sanjuan, P.-W. Wang, P. Cassata, B. Garilli, O. Ilbert, V. Le Brun, B. C. Lemaux, D. Maccagni, L. Tresse, S. Bardelli, T. Contini, S. Charlot, O. Cucciati, A. Fontana, M. Giavalisco, J.-P. Kneib, M. Salvato, Y. Taniguchi, D. Vergani, G. Zamorani, and E. Zucca

Subjects
Physics, Stellar mass, 010308 nuclear & particles physics, Star formation, Galaxies: high-redshift, Context (language use), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy merger, Mass ratio, Galaxies: formation, Space and Planetary Science, 01 natural sciences, Redshift, Galaxy, Photometry (optics), 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Context. The mass assembly of galaxies can proceed through different physical processes. Here we report on the spectroscopic identification of close physical pairs of galaxies at redshi fts 2. z< 4 and discuss the impact of major mergers in shaping galaxies at these early cosmological times. Aims. We aim to identify and characterize close physical pairs of galaxies destined to merge and use their properties to infer t he contribution of merging processes to the early mass assembly of galaxies. Methods. We search for galaxy pairs with a transverse separation rp ≤ 25 h −1 kpc and a velocity differencev≤ 500 km s −1 using the VIMOS VLT Deep Survey (VVDS) and early data from the VIMOSUltra Deep Survey (VUDS) that comprise a sample of 1111 galaxies with spectroscopic redshifts measurements at redshifts 1.8≤ z≤ 4 in the COSMOS, ECDFS, and VVDS-02h fields. We analyse their spectra and associated visible and near-infr ared photometry to assess the main properties of merging galaxies that have an average stellar mass M⋆ = 2.3× 10 10 M⊙ at these redshifts. Results. Using the 12 physical pairs found in our sample we obtain a firs t estimate of the merger fraction at these rdshifts, fmerg∼ (15− 20)%. The pair separations indicate that these pairs will merge within 1 Gyr, on average, with each producing a more massive galaxy by the time the cosmic star formation peaks at z∼ 1− 2. From the average mass ratio between galaxies in the pairs, the stellar mass of the resulting galaxy after merging will be∼ 60% larger than the most massive galaxy in the pair before merging. We conclude that major merging of galaxy pairs is on-going at 2. z< 4 and significantly contributing to the major assembly phase of galaxies at this early epoch.

Published
2014

138. Radio properties of the Shapley Concentration -- I. The Abell cluster A3556

Author

Tiziana Venturi, Richard W. Hunstead, S. Bardelli, and Raffaella Morganti

Subjects
Physics, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, X-shaped radio galaxy, Abell 2744, Space and Planetary Science, Elliptical galaxy, Brightest cluster galaxy, Molonglo Observatory Synthesis Telescope, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Luminosity function (astronomy)
Abstract

We have imaged the portion of the Shapley Concentration core surrounding the cluster A3556 at wavelengths of 36 cm with the Molonglo Observatory Synthesis Telescope (MOST), and at 22 and 13 cm with the Australia Telescope Compact Array (ATCA). We have defined a radio sample of 112 radio sources at 22 cm. Cross-correlation with optical catalogues allowed the identification of 29 radio sources, nine of which belong to A3556. The radio and optical properties of A3556 have been studied in detail. Two extended radio sources are associated with cluster members, i.e. a narrow-angle-tail source located at a projected distance of O.06RA from the centre, possibly in the late stages of its existence, and a wide-angle-tail source at the periphery of the cluster. We also performed a statistical analysis of the cluster properties. The optical luminosity function shows that the cluster has an excess of bright optical galaxies. In agreement with well-established results, we found that the probability of radio emission increases for brighter galaxies. Furthermore, our radio luminosity function and those obtained for elliptical galaxies located in different environments (poor groups and rich clusters) are very similar, implying that the peculiar dynamical state of A3556 has no influence on the radio emission properties of the cluster galaxies.

Published
1997
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139. The VIMOS VLT Deep Survey final data release: a spectroscopic sample of 35 016 galaxies and AGN out to z ~ 6.7 selected with 17.5 \u2264 iAB \u2264 24.75

Author

O. Le Fxe8vre, P. Cassata, O. Cucciati, B. Garilli, O. Ilbert, V. Le Brun, D. Maccagni, C. Moreau, M. Scodeggio, L. Tresse, G. Zamorani, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, M. Bondi, A. Bongiorno, D. Bottini, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. de la Torre, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, A. Iovino, B. Lemaux, H.J. McCracken, B. Marano, C. Marinoni, A. Mazure, Y. Mellier, R. Merighi, P. Merluzzi, S. Paltani, R. Pello, A. Pollo, L. Pozzetti, R. Scaramella, and D. Vergan

Published
2013

141. The dependence of Galactic outflows on the properties and orientation of zCOSMOS galaxies at z ~ 1

Author

A. Cappi, E. Zucca, Alvio Renzini, Pascal Oesch, Masaomi Tanaka, C. Knobel, V. Presotto, Anton M. Koekemoer, Gianni Zamorani, K. Kovac, P. Nair, S. de la Torre, V. Mainieri, Angela Bongiorno, M. Bolzonella, Jean-Paul Kneib, Lucia Pozzetti, Daniela Vergani, M. Scodeggio, J. F. Le Borgne, A. Iovino, E. Hardmeier, P. Kampczyk, Thierry Contini, B. Garilli, Roser Pello, Rongmon Bordoloi, John D. Silverman, M. Mignoli, O. Le Fèvre, S. Bardelli, Michele Moresco, Andrea Cimatti, V. Le Brun, Lidia Tasca, C. M. Carollo, Christian Maier, P. Franzetti, F. Lamareille, Y. Peng, E. Perez Montero, Olga Cucciati, Karina Caputi, Simon J. Lilly, Laurence Tresse, Graziano Coppa, L. de Ravel, Bordoloi, R., Lilly, S.J., Hardmeier, E., Contini, T., Kneib, J.-P., Fevre, O. Le, Mainieri, V., Renzini, A., Scodeggio, M., Zamorani, G., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Carollo, C.M., Cucciati, O., De La Torre, S., De Ravel, L., Garilli, B., Iovino, A., Kampczyk, P., Kovač, K., Knobel, C., Lamareille, F., Borgne, J.-F. Le, Brun, V. Le, Maier, C., Mignoli, M., Oesch, P., Pello, R., Peng, Y., Perez Montero, E., Presotto, V., Silverman, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., Cappi, A., Cimatti, A., Coppa, G., Franzetti, P., Koekemoer, A., Moresco, M., Nair, P., and Pozzetti, L.

Subjects
Physics, Nuclear and High Energy Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Absorption spectroscopy, Star formation, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Mass loading, ultraviolet: ISM, Galaxy, Spectral line, Orientation (vector space), Space and Planetary Science, galaxies: high-redshift, Astrophysics::Solar and Stellar Astrophysics, intergalactic medium, galaxies: evolution, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present an analysis of cool outflowing gas around galaxies, traced by MgII absorption lines in the co-added spectra of a sample of 486 zCOSMOS galaxies at 1 < z < 1.5. These galaxies span a range of stellar masses (9.45< log[M*/Msun] 5-7 Msun/yr and a mass loading factor (�� = dMout/dt /SFR) comparable to the star formation rates of the galaxies., 12 pages, 14 figures, ApJ submitted

Published
2013

142. The role of major mergers in shaping galaxies at 2<z<4 in the VUDS and VVDS surveys

Author

L. A. M. Tasca, O. Le Fevre, C. Lopez-Sanjuan, P.-W. Wang, P. Cassata, B. Garilli, O. Ilbert, V. Le Brun, B. C. Lemaux, D. Maccagni, L. Tresse, S. Bardelli, T. Contini, O. Cucciati, A. Fontana, M. Giavalisco, J.-P. Kneib, M. Salvato, Y. Taniguchi, D. Vergani, G. Zamorani, and E. Zucca

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

The mass assembly of galaxies can proceed through different physical processes. Here we report on the spectroscopic identification of close physical pairs of galaxies at redshifts 2, Comment: 12 pages, 12 figures, submitted to A&A

Published
2013

143. Proto-groups at 1.8 < z < 3 in the zCOSMOS-deep Sample

Author

Laurence Tresse, Preethi Nair, C. Diener, Anton M. Koekemoer, S. Bardelli, J. F. Le Borgne, Angela Bongiorno, C. Knobel, Gianni Zamorani, Andrea Cimatti, V. Mainieri, K. Kovac, Alvio Renzini, M. Scodeggio, M. Bolzonella, Graziano Coppa, Jean-Paul Kneib, A. Iovino, E. Zucca, C. López-Sanjuan, Christian Maier, Lucia Pozzetti, Daniela Vergani, Thierry Contini, John D. Silverman, A. Cappi, Bianca Garilli, Simon J. Lilly, E. Perez Montero, Karina Caputi, L. de Ravel, Y. Peng, Rongmon Bordoloi, S. de la Torre, V. Presotto, V. Le Brun, N. Z. Scoville, O. Le Fèvre, Michele Moresco, Niraj Welikala, F. Lamareille, Lidia Tasca, Gerard Lemson, Masayuki Tanaka, C. M. Carollo, M. Mignoli, P. Kampczyk, R. Pello, P. Franzetti, H. J. McCracken, and Olga Cucciati

Subjects
SDSS, 010504 meteorology & atmospheric sciences, Sample (material), Astrophysics, TO 2.5, MASS, 01 natural sciences, galaxies: groups: general, galaxies: high-redshift, SATELLITE GALAXIES, 0103 physical sciences, Satellite galaxy, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, IDENTIFICATION, Epoch (reference date), Astronomy and Astrophysics, GROUP CATALOG, Redshift survey, STAR-FORMATION HISTORY, Redshift, Galaxy, EVOLUTION, Space and Planetary Science, Physical space, Halo, HIGH-REDSHIFT, CLUSTERS, catalogs
Abstract

We identify 42 "candidate groups" lying between 1.8

Published
2013
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144. Spot the difference - Impact of different selection criteria on observed properties of passive galaxies in zCOSMOS-20k sample

Author

O. Cucciati, S. J. Lilly, Christian Maier, E. Le Floc'h, D. Vergani, John D. Silverman, C. Lopez-Sanjuan, S. de la Torre, Nick Scoville, F. Lamareille, A. Cappi, A. Cimatti, Luke A. Barnes, Y. Peng, Enrique Perez-Montero, Alvio Renzini, Katarina Kovac, P. Kampczyk, C. M. Carollo, L. A. M. Tasca, J. F. Le Borgne, Masaomi Tanaka, Michele Moresco, Angela Bongiorno, A. Iovino, Pradip Nair, L. de Ravel, V. Presotto, Claudia Scarlata, K. Caputi, E. Zucca, S. Bardelli, T. Contini, G. Zamorani, J. P. Kneib, Niraj Welikala, O. Le Fevre, L. Tresse, Anton M. Koekemoer, Marco Scodeggio, C. Knobel, Rongmon Bordoloi, M. Bolzonella, C. Diener, V. Le Brun, Lucia Pozzetti, B. Garilli, P. Franzetti, Vincenzo Mainieri, Pascal Oesch, R. Pello, M. Mignoli, H. J. McCracken, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 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 Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Moresco M., Pozzetti L., Cimatti A., Zamorani G., Bolzonella M., Lamareille F., Mignoli M., Zucca E., Lilly S. J., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bardelli S., Bongiorno A., Caputi K., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Kovac K., Le Borgne J.-F., Le Brun V., Maier C., Pelló R., Peng Y., Perez-Montero E., Presotto V., Silverman J. D., Tanaka M., Tasca L., Tresse L., Vergani D., Barnes L., Bordoloi R., Cappi A., Diener C., Koekemoer A. M., Le Floc'h E., López-Sanjuan C., McCracken H. J., Nair P., Oesch P., Scarlata C., Scoville N., Welikala N., and Astronomy

Subjects
ACTIVE GALACTIC NUCLEI, Galaxies: fundamental parameters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Galaxies: statistics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Sample (material), Population, FOS: Physical sciences, PHYSICAL-PROPERTIES, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surveys, 01 natural sciences, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, education, PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Selection (genetic algorithm), REDSHIFT SURVEY, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Cosmology: observations, Galaxies: high-redshift, Galaxies: statistics, Large-scale structure of Universe, Galaxies: evolution, Astronomy and Astrophysics, VLT DEEP SURVEY, Galaxy, 13. Climate action, Space and Planetary Science, Outlier, STELLAR MASS FUNCTION, DIGITAL SKY SURVEY, Spectral energy distribution, 10K-BRIGHT SPECTROSCOPIC SAMPLE, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the analysis of photometric, spectroscopic, and morphological properties for differently selected samples of passive galaxies up to z=1 extracted from the zCOSMOS-20k spectroscopic survey. This analysis intends to explore the dependence of galaxy properties on the selection criterion adopted, study the degree of contamination due to star-forming outliers, and provide a comparison between different commonly used selection criteria. We extracted from the zCOSMOS-20k catalog six different samples of passive galaxies, based on morphology, optical colors, specific star-formation rate, a best fit to the observed spectral energy distribution, and a criterion that combines morphological, spectroscopic, and photometric information. The morphological sample has the higher percentage of contamination in colors, specific star formation rate and presence of emission lines, while the red & passive ETGs sample is the purest, with properties mostly compatible with no star formation activity; however, it is also the less economic criterion in terms of information used. The best performing among the other criteria are the red SED and the quiescent ones, providing a percentage of contamination only slightly higher than the red & passive ETGs criterion (on average of a factor of ~2) but with absolute values of the properties of contaminants still compatible with a red, passively evolving population. We also provided two revised definitions of early type galaxies based on restframe color-color and color-mass criteria, that better reproduce the observed bimodalities. The analysis of the number densities shows evidences of mass-assembly downsizing, with galaxies at 10.25, Comment: 20 pages, 14 figures, 2 tables, accepted for publication in A\&A

Published
2013
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145. Erratum: The Herschel PEP/HerMES Luminosity Function - I. Probing the Evolution of PACS selected Galaxies to z = 4

Author

P. Chania, G. Mainetti, M. Bethermin, I. Ṕerez-Fournon, Matthew Joseph Griffin, L. Vigroux, H. Aussel, J. J. Bock, Andreas Papageorgiou, Vincenzo Mainieri, Anthony J. Smith, A. Conley, Benjamin Magnelli, Bruno Altieri, Asantha Cooray, Marcella Carollo, Raanan Nordon, V. Buat, Linda J. Tacconi, V. Arumugam, B. O'Halloran, E. Ibar, Alberto Franceschini, Alexandre Amblard, Francesca Pozzi, S. Bardelli, David J. Rosario, Bruno Maffei, Dimitra Rigopoulou, Mattia Vaccari, G. Wright, K. G. Isaak, Simon J. Lilly, Lucia Marchetti, Dieter Lutz, S. Berta, Ángel Bongiovanni, Albrecht Poglitsch, Michael Rowan-Robinson, I. Valtchanov, Alvaro Iribarrem, E. Zucca, Michael Pohlen, C. K. Xu, Marco Scodeggio, P. Popesso, Guilaine Lagache, G. Rodighiero, Thierry Contini, M. J. Page, Emanuele Daddi, Eckhard Sturm, Roberto Maiolino, S. C. Madden, N. M. Förster Schreiber, Jason Glenn, E. Le Floc'h, David L. Shupe, Lucia Pozzetti, Michael Zemcov, Alvio Renzini, M. Magliocchetti, Eli Dwek, N. Castro-Rodŕlguez, Douglas Scott, Louis Levenson, C. D. Dowell, R. Genzel, D. Elbaz, Nick Seymour, Rob Ivison, Jamie Stevens, Andrea Cimatti, Antonio Cava, Evanthia Hatziminaoglou, H. T. Nguyen, Nanyao Y. Lu, M. Symeonidis, Paola Andreani, Alessandro Boselli, O. Le Fevre, K. E. Tugwell, L. Riguccini, P. Panuzzo, A. Ṕerez Garćla, G. Zamorani, Chris Pearson, M. Sánchez-Portal, David L. Clements, Steve Eales, Denis Burgarella, L. Monaco, Ivan Delvecchio, J. Cepa, H. Doḿlnguez-Śanchez, M. T. Sargent, Benjamin L. Schulz, S. J. Oliver, Lian-Tao Wang, Carlotta Gruppioni, Isaac Roseboom, Markos Trichas, and O. Ilbert

Subjects
Luminous infrared galaxy, Physics, Radio galaxy, Física atmosférica, Astronomy, Astronomy and Astrophysics, Astrophysics, Disc galaxy, Galaxy, Space and Planetary Science, Galaxy group, Galaxy formation and evolution, Elliptical galaxy, Luminosity function (astronomy)
Abstract

This is an erratum to the paper ‘The Herschel PEP/HerMES Luminosity Function – I: Probing the Evolution of PACS selected Galaxies to z ≃ 4’, by Gruppioni et al., published in MNRAS, 432, 23 (2013).

Published
2013

146. ENVIRONMENTAL EFFECTS IN THE INTERACTION AND MERGING OF GALAXIES IN zCOSMOS

Author

P. Kampczyk, S. J. Lilly, L. de Ravel, O. Le Fèvre, M. Bolzonella, C. M. Carollo, C. Diener, C. Knobel, K. Kovač, C. Maier, A. Renzini, M. T. Sargent, D. Vergani, U. Abbas, S. Bardelli, A. Bongiorno, R. Bordoloi, K. Caputi, T. Contini, G. Coppa, O. Cucciati, S. de la Torre, P. Franzetti, B. Garilli, A. Iovino, J.-P. Kneib, A. M. Koekemoer, F. Lamareille, J.-F. Le Borgne, V. Le Brun, A. Leauthaud, V. Mainieri, M. Mignoli, R. Pello, Y. Peng, E. Perez Montero, E. Ricciardelli, M. Scodeggio, J. D. Silverman, M. Tanaka, L. Tasca, L. Tresse, G. Zamorani, E. Zucca, D. Bottini, A. Cappi, P. Cassata, A. Cimatti, M. Fumana, L. Guzzo, J. Kartaltepe, C. Marinoni, H. J. McCracken, P. Memeo, B. Meneux, P. Oesch, C. Porciani, L. Pozzetti, R. Scaramella, AUTRES, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Chicago, Laboratoire Léon Brillouin (LLB - UMR 12), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astrofisico di Torino (OATo), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], 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), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Ecole Polytechnique Fédérale de Lausanne (EPFL), Institut de recherche en astrophysique et planétologie (IRAP), California Institute of Technology (CALTECH), European Southern Observatory (ESO), Hunan Normal University (HNU), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), National Optical Astronomy Observatory (NOAO), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astronomy, 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Hunan Normal University, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Kampczyk P., Lilly S. J., de Ravel L., Le Fèvre O., Bolzonella M., Carollo C. M., Diener C., Knobel C., Kovac K., Maier C., Renzini A., Sargent M. T., Vergani D., Abbas U., Bardelli S., Bongiorno A., Bordoloi R., Caputi K., Contini T., Coppa G., Cucciati O., de la Torre S., Franzetti P., Garilli B., Iovino A., Kneib J.-P., Koekemoer A. M., Lamareille F., Le Borgne J.-F., Le Brun V., Leauthaud A., Mainieri V., Mignoli M., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Scodeggio M., Silverman J. D., Tanaka M., Tasca L., Tresse L., Zamorani G., Zucca E., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Guzzo L., Kartaltepe J., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., and Scaramella R.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, galaxies: starburst, MORPHOLOGICAL TRANSFORMATION, Astrophysics, Kinematics, Astrophysics::Cosmology and Extragalactic Astrophysics, STAR-FORMATION RATES, MERGER RATE EVOLUTION, 01 natural sciences, SIMILAR-TO 1, galaxies: evolution, galaxies: general, galaxies: interactions, Astronomy and Astrophysics, Space and Planetary Science, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Fraction (mathematics), education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, QB, Physics, education.field_of_study, FORMATION HISTORY, Star formation, CLOSE PAIRS, Cosmology: observations, Galaxies: high-redshift, Galaxies: statistics, Large-scale structure of Universe, CNOC2 REDSHIFT SURVEY, DISK GALAXIES, Environmental variation, Galaxy, Redshift, COSMOS FIELD, DIGITAL SKY SURVEY, Irregular galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

(Abridged) We analyze the environments and galactic properties (morphologies and star-formation histories) of a sample of 153 close kinematic pairs in the redshift range 0.2 < z < 1 identified in the zCOSMOS-bright 10k spectroscopic sample of galaxies. Correcting for projection effects, the fraction of close kinematic pairs is three times higher in the top density quartile than in the lowest one. This translates to a three times higher merger rate because the merger timescales are shown, from mock catalogues based on the Millennium simulation, to be largely independent of environment once the same corrections for projection is applied. We then examine the morphologies and stellar populations of galaxies in the pairs, comparing them to control samples that are carefully matched in environment so as to remove as much as possible the well-known effects of environment on the properties of the parent population of galaxies. Once the environment is properly taken into account in this way, we find that the early-late morphology mix is the same as for the parent population, but that the fraction of irregular galaxies is boosted by 50-75%, with a disproportionate increase in the number of irregular-irregular pairs (factor of 4-8 times), due to the disturbance of disk galaxies. Future dry-mergers, involving elliptical galaxies comprise less than 5% of all close kinematic pairs. In the closest pairs, there is a boost in the specific star-formation rates of star-forming galaxies of a factor of 2-4, and there is also evidence for an increased incidence of post star-burst galaxies. Although significant for the galaxies involved, the "excess" star-formation associated with pairs represents only about 5% of the integrated star-formation activity in the parent sample. Although most pair galaxies are in dense environments, the effects of interaction appear to be largest in the lower density environments., 38 pages, 17 figures, submitted to ApJ

Published
2013
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147. The VIMOS VLT Deep Survey final data release: a spectroscopic sample of 35 016 galaxies and AGN out to z ~ 6.7 selected with 17.5 ≤ i_AB ≤ 24.75

Author

O. Le Fèvre, P. Cassata, O. Cucciati, B. Garilli, O. Ilbert, V. Le Brun, D. Maccagni, C. Moreau, M. Scodeggio, L. Tresse, G. Zamorani, C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, M. Bondi, A. Bongiorno, D. Bottini, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, S. de la Torre, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, A. Iovino, B. Lemaux, C. López-Sanjuan, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure†, Y. Mellier, R. Merighi, P. Merluzzi, S. Paltani, R. Pellò, A. Pollo, L. Pozzetti, R. Scaramella, L. Tasca, D. Vergani, G. Vettolani, A. Zanichelli, E. Zucca, 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 Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto di Radioastronomia [Bologna] (IRA), 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of Edinburgh, National Taiwan Normal University (NTNU), Universidad Andrés Bello [Santiago] (UNAB), INAF - Osservatorio Astronomico di Brera (OAB), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Uniwersytet Jagielloński w Krakowie = Jagiellonian University (UJ), INAF - Osservatorio Astronomico di Roma (OAR), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-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), Surace, Christian, Early phases of galaxy evolution - EARLY - - EC:FP7:ERC2011-04-01 - 2016-03-31 - 268107 - VALID, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Le Fèvre O., Cassata P., Cucciati O., Garilli B., Ilbert O., Le Brun V., Maccagni D., Moreau C., Scodeggio M., Tresse L., Zamorani G., Adami C., Arnouts S., Bardelli S., Bolzonella M., Bondi M., Bongiorno A., Bottini D., Cappi A., Charlot S., Ciliegi P., Contini T., de la Torre S., Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Iovino A., Lemaux B., López-Sanjuan C., McCracken H. J., Marano B., Marinoni C., Mazure A., Mellier Y., Merighi R., Merluzzi P., Paltani S., Pellò R., Pollo A., Pozzetti L., Scaramella R., Tasca L., Vergani D., Vettolani G., Zanichelli A., and Zucca E.

Subjects
Large-scale structure of Universe, media_common.quotation_subject, Sample (statistics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Galaxies: formation, 01 natural sciences, Cosmology: observation, Spectral line, Galaxie, LARGE SCALE STRUCTURE OF THE UNIVERSE, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, evolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Cosmology: observations, Galaxies: evolution, Galaxies: high-redshift, Astronomy and Astrophysics, Space and Planetary Science, Physics, 010308 nuclear & particles physics, high redshift, formation, Redshift, Universe, Galaxy, Stars, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Magnitude (astronomy), Data release
Abstract

Submitted 30 June 2013, Accepted 22 August 2013. Updated with published version; International audience; Context. Deep representative surveys of galaxies at different epochs are needed to make progress in understanding galaxy evolution. Aims. We describe the completed VIMOS VLT Deep Survey and the final data release of 35 016 galaxies and type-I AGN with measured spectro-scopic redshifts covering all epochs up to redshiftz∼6.7, in areas from 0.142 to 8.7 square degrees, and volumes from 0.5×106to 2×107h−3Mpc3. Methods. We selected samples of galaxies based solely on their i-band magnitude reaching iAB=24.75. Spectra were obtained with VIMOS on the ESO-VLT integrating 0.75 h, 4.5 h, and 18 h for the Wide, Deep, and Ultra-Deep nested surveys, respectively. We demonstrate that any “redshift desert” can be crossed successfully using spectra covering 3650 ≤λ≤9350 Å. A total of 1263 galaxies were again observed independently within the VVDS and from the VIPERS and MASSIV surveys. They were used to establish the redshift measurements reliability, to assess completeness in the VVDS sample, and to provide a weighting scheme taking the survey selection function into account. We describe the main properties of the VVDS samples, and the VVDS is compared to other spectroscopic surveys in the literature. Results. In total we have obtained spectroscopic redshifts for 34 594 galaxies, 422 type-I AGN, and 12 430 Galactic stars. The survey enabled identifying galaxies up to very high redshifts with 4669 redshifts in 1≤ z spec ≤2, 561 in 2≤z spec ≤3, and 468 with z spec >3, and specific populations like Lyman-α emitters were identified out to z = 6.62. We show that the VVDS occupies a unique place in the parameter space defined by area, depth, redshift coverage, and number of spectra. Conclusions. The VIMOS VLT Deep Survey provides a comprehensive survey of the distant universe, covering all epochs since z∼6, or more than 12 Gyr of cosmic time, with a uniform selection, which is the largest such sample to date. A wealth of science results derived from the VVDS have shed new light on the evolution of galaxies and AGN and on their distribution in space over this large cosmic time. The VVDS further demonstrates that large deep spectroscopic redshift surveys over all these epochs in the distant Universe are a key tool to observational cosmology.To enhance the legacy value of the survey, a final public release of the complete VVDS spectroscopic redshift sample is available at http://cesam.lam.fr/vvds.

Published
2013
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148. Hidden starbursts and active galactic nuclei at 0 < z < 4 from the Herschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback (Corrigendum)

Author

S. Bardelli, E. Zucca, Laurence Tresse, Lori M. Lubin, O. Le Fevre, Elizabeth J. McGrath, G. Zamorani, Paolo Ciliegi, D. D. Kocevski, O. Ilbert, G. K. Squires, Brian C. Lemaux, Paolo Cassata, E. Le Floc'h, and Roy R. Gal

Subjects
Physics, Luminous infrared galaxy, Active galactic nucleus, 010308 nuclear & particles physics, Radio galaxy, Astronomy, Astronomy and Astrophysics, Quasar, Astrophysics, 01 natural sciences, Space and Planetary Science, Galaxy group, 0103 physical sciences, Galaxy formation and evolution, Elliptical galaxy, Disc, 010303 astronomy & astrophysics
Published
2016
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149. Size evolution of star-forming galaxies with 2 <z< 4.5 in the VIMOS Ultra-Deep Survey

Author

Mauro Giavalisco, O. Le Fèvre, B. Ribeiro, Ricardo Amorín, Nimish P. Hathi, James S. Dunlop, Laurence Tresse, Anton M. Koekemoer, E. Zucca, D. Maccagni, Janine Pforr, S. Bardelli, Bianca Garilli, Adriano Fontana, Brian C. Lemaux, Lidia Tasca, G. Zamorani, and Paolo Cassata

Subjects
Effective radius, Physics, 010308 nuclear & particles physics, Star formation, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Redshift, Galaxy, Galaxies: structure, Space and Planetary Science, Stars, 0103 physical sciences, Galaxy formation and evolution, Spectral energy distribution, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We measure galaxy sizes on a sample of $\sim1200$ galaxies with confirmed spectroscopic redshifts $2 \leq z_{spec} \leq 4.5$ in the VIMOS Ultra Deep Survey (VUDS), representative of star-forming galaxies with $i_\mathrm{AB} \leq 25$. We first derive galaxy sizes applying a classical parametric profile fitting method using GALFIT. We then measure the total pixel area covered by a galaxy above a given surface brightness threshold, which overcomes the difficulty of measuring sizes of galaxies with irregular shapes. We then compare the results obtained for the equivalent circularized radius enclosing 100\% of the measured galaxy light $r_T^{100}$ to those obtained with the effective radius $r_{e,\mathrm{circ}}$ measured with GALFIT. We find that the sizes of galaxies computed with our non-parametric approach span a large range but remain roughly constant on average with a median value $r_T^{100}\sim2.2$ kpc for galaxies with $2, Comment: 22 pages, 20 figures (+3 in appendix), submitted to A&A

Published
2016
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150. Effect of the star formation histories on theSFR-M∗relation atz≥ 2

Author

S. Paltani, James Dunlop, Nimish P. Hathi, Daniel Schaerer, Thierry Contini, B. Ribeiro, V. Sommariva, Marco Scodeggio, Daniela Vergani, Laurence Tresse, C. Lopez-Sanjuan, Nick Scoville, Anton M. Koekemoer, M. Giavalisco, Peter Capak, V. Le Brun, O. Ilbert, Andrea Grazian, Marco Castellano, Janine Pforr, Alessandro Cimatti, Adriano Fontana, Mara Salvato, E. Zucca, Brian C. Lemaux, O. Cucciati, G. Zamorani, S. de la Torre, D. Maccagni, L. A. M. Tasca, P. W. Wang, Yannick Mellier, Lucia Guaita, Paolo Cassata, Rajat M. Thomas, Letizia P. Cassarà, S. Bardelli, A. Durkalec, Margherita Talia, B. Garilli, Eros Vanzella, Stéphane Charlot, Yoshi Taniguchi, Laura Pentericci, Ricardo Amorín, O. Le Fevre, Sotiria Fotopoulou, 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), European Project: 606847,EC:FP7:SPA,FP7-SPACE-2013-1,DUSTPEDIA(2014), ITA, USA, GBR, FRA, DEU, ESP, CHL, JPN, GRC, CHE, Cassarà, L.P., Maccagni, D., Garilli, B., Scodeggio, M., Thomas, R., Le Fèvre, O., Zamorani, G., Schaerer, D., Lemaux, B.C., Cassata, P., Le Brun, V., Pentericci, L., Tasca, L.A.M., Vanzella, E., Zucca, E., Amorín, R., Bardelli, S., Castellano, M., Cimatti, A., Cucciati, O., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Paltani, S., Ribeiro, B., Sommariva, V., Talia, M., Tresse, L., Vergani, D., Capak, P., Charlot, S., Contini, T., De La Torre, S., Dunlop, J., Fotopoulou, S., Guaita, L., Koekemoer, A., López-Sanjuan, C., Mellier, Y., Pforr, J., Salvato, M., Scoville, N., Taniguchi, Y., Wang, P.W., Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Stellar mass, Stellar population, Extinction (astronomy), Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxies: formation, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Galaxies: evolution, Galaxies: high-redshift, Galaxies: star formation, Astronomy and Astrophysics, Space and Planetary Science, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysic, Redshift, Galaxy, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics
Abstract

We investigate the effect of different star formation histories (SFHs) on the relation between stellar mass (M∗) and star formation rate (SFR) using a sample of galaxies with reliable spectroscopic redshift zspec> 2 drawn from the VIMOS Ultra-Deep Survey (VUDS). We produce an extensive database of dusty model galaxies, calculated starting from a new library of single stellar population (SSPs) models, weighted by a set of 28 different star formation histories based on the Schmidt function, and characterized by different ratios of the gas infall timescale τinfall to the star formation efficiency ν. Dust extinction and re-emission were treated by means of the radiative transfer calculation. The spectral energy distribution (SED) fitting technique was performed by using GOSSIP+, a tool able to combine both photometric and spectroscopic information to extract the best value of the physical quantities of interest, and to consider the intergalactic medium (IGM) attenuation as a free parameter. We find that the main contribution to the scatter observed in the SFR-M∗ plane is the possibility of choosing between different families of SFHs in the SED fitting procedure, while the redshift range plays a minor role. The majority of the galaxies, at all cosmic times, are best fit by models with SFHs characterized by a high τinfall/ν ratio. We discuss the reliability of a low percentage of dusty and highly star-forming galaxies in the context of their detection in the far infrared (FIR).

Published
2016
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