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arXiv: 0909.4674
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The zCOSMOS survey: the role of the environment in the evolution of the luminosity function of different galaxy types
E. Zucca 1, S. Bardelli 2, M. Bolzonella 3, G. Zamorani 4, O. Ilbert 5, L. Pozzetti 2, M. Mignoli 4, K. Kovac 4, S. Lilly 4, L. Tresse 5, L. Tasca 5, P. Cassata 4, C. Halliday, D. Vergani 6, K. Caputi 4, C. M. Carollo 7, T. Contini 8, J. P. Kneib 8, O. LeFevre 5, V. Mainieri 4, A. Renzini 4, M. Scodeggio 9, A. Bongiorno 3, G. Coppa 4, O. Cucciati 10, S. delaTorre, L. deRavel, P. Franzetti 4, B. Garilli 4, A. Iovino 4, P. Kampczyk 4, C. Knobel 4, F. Lamareille 8, J. F. LeBorgne 8, V. Lebrun 5, C. Maier 4, R. Pello', Y. Peng 11, E. Perez-Montero 8, E. Ricciardelli 4, J. D. Silverman 4, M. Tanaka 12, U. Abbas 4, D. Bottini 4, A. Cappi 13, A. Cimatti 4, L. Guzzo 4, A. M. Koekemoer 14, A. Leauthaud 5, D. Maccagni 4, C. Marinoni 15, H. J. McCracken 16, P. Memeo 4, B. Meneux 5, M. Moresco, P. Oesch 4, C. Porciani 4, R. Scaramella 4, S. Arnouts 5, H. Aussel 4, P. Capak 17, J. Kartaltepe 4, M. Salvato 17, D. Sanders 18, N. Scoville 19, Y. Taniguchi 4, D. Thompson 20
(2009-09-25)
(Abridged) We studied the evolution in the B band luminosity function to z~1 in the zCOSMOS 10k sample, for which both accurate galaxy classifications and a detailed description of the local density field are available. The global LF exhibits a brightening of ~0.7 mag in M* from z~0.2 to z~0.9. At low z, late types dominate at faint magnitudes, while the bright end is populated mainly by early types. At higher z, late-type galaxies evolve significantly and, at z~1, the contribution from the various types to the bright end of the LF is comparable. The evolution for early types is in both luminosity and normalization. A similar behaviour is exhibited by late types, but with an opposite trend for the normalization. Studying the role of the environment, we find that the global LF of galaxies in overdense regions has always a brighter M* and a flatter slope. In low density environments, the main contribution to the LF is from blue galaxies, while for high density environments there is an important contribution from red galaxies to the bright end. The differences between the global LF in the two environments are not due to only a difference in the relative numbers of red and blue galaxies, but also to their relative luminosity distributions: the value of M* for both types in underdense regions is always fainter than in overdense environments. The "specular" evolution of late- and early-type galaxies is consistent with a scenario where a part of blue galaxies is transformed in red galaxies with increasing cosmic time, without significant changes in the fraction of intermediate-type galaxies. The bulk of this tranformation in overdense regions probably happened before z~1, while it is still ongoing at lower z in underdense environments.
1:  Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Brera (INAF)
Istituto Nazionale di Astrofisica
2:  INAF- Osservatorio Astronomico di Bologna (INAF)
INAF
3:  Università di Bologna, Dipartimento di Astronomia
Università degli studi di Bologna
4:  Autres
AUTRE
5:  Laboratoire d'Astrophysique de Marseille (LAM)
CNRS : UMR6110 – INSU – Université de Provence - Aix-Marseille I
6:  INAF, Osservatorio Astrofisico di Arcetri, Largo
Osservatorio Astrofisico di ArcetI
7:  The University of Chicago
Dept of the Geophysical Sciences
8:  Laboratoire Astrophysique de Toulouse-Tarbes (LATT)
CNRS : UMR5572 – INSU – Observatoire Midi-Pyrénées – Université Paul Sabatier [UPS] - Toulouse III
9:  INAF- Milano
INAF
10:  Dipartimento di Fisica
Università di Milano-Bicocca – Università degli studi di Milano
11:  Laboratory for Climate Studies
Laboratory for Climate Studies
12:  Tokai University
Tokai University
13:  Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo)
INAF
14:  Space Telescope Science Institute (STSI)
Space Telescope Science Institute
15:  Centre de Physique Théorique (CPT)
CNRS : FR2291 – Université de Provence - Aix-Marseille I – Université de la Méditerranée - Aix-Marseille II – Université Sud Toulon Var
16:  Institut d'Astrophysique de Paris (IAP)
CNRS : UMR7095 – INSU – Université Pierre et Marie Curie [UPMC] - Paris VI
17:  Max Planck Institut für Astronomie (MPIA)
Max Planck Institut für Astronomie
18:  Materials & Process technology
BOEING Company
19:  California Institute of Technology (Caltech)
California Institute of Technology
20:  Sea Mammal Research Unit
St Andrews
Subject :  Physics/Astrophysics/Cosmology and Extra-Galactic Astrophysics
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http://fr.arXiv.org/abs/0909.4674
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From: Elizabeth Bernardo <>
Submitted on: Sunday, 4 October 2009 11:49:07
Updated on: Sunday, 4 October 2009 11:49:07