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The zCOSMOS survey: the role of the environment in the evolution of the luminosity function of different galaxy types

Zucca, E. and Bardelli, S. and Bolzonella, M. and Zamorani, G. and Ilbert, O. and Pozzetti, L. and Mignoli, M. and Kovač, K. and Lilly, S. and Tresse, L. and Tasca, L. and Cassata, P. and Halliday, C. and Vergani, D. and Caputi, K. and Carollo, C. M. and Contini, T. and Kneib, J.-P. and Le Fèvre, O. and Mainieri, V. and Renzini, A. and Scodeggio, M. and Bongiorno, A. and Coppa, G. and Cucciati, O. and de la Torre, S. and de Ravel, L. and Franzetti, P. and Garilli, B. and Iovino, A. and Kampczyk, P. and Knobel, C. and Lamareille, F. and Le Borgne, J.-F. and Le Brun, V. and Maier, C. and Pellò, R. and Peng, Y. and Pérez-Montero, E. and Ricciardelli, E. and Silverman, J. D. and Tanaka, M. and Abbas, U. and Bottini, D. and Cappi, A. and Cimatti, A. and Guzzo, L. and Koekemoer, A. M. and Leauthaud, A. and Maccagni, D. and Marinoni, C. and McCracken, H. J. and Memeo, P. and Meneux, B. and Moresco, M. and Oesch, P. and Porciani, C. and Scaramella, R. and Arnouts, S. and Aussel, H. and Capak, P. and Kartaltepe, J. and Salvato, M. and Sanders, D. and Scoville, N. and Taniguchi, Y. and Thompson, D. (2009) The zCOSMOS survey: the role of the environment in the evolution of the luminosity function of different galaxy types. Astronomy and Astrophysics, 508 (3). pp. 1217-1234. ISSN 0004-6361. doi:10.1051/0004-6361/200912665.

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Aims. An unbiased and detailed characterization of the galaxy luminosity function (LF) is a basic requirement in many astrophysical issues: it is of particular interest in assessing the role of the environment in the evolution of the LF of different galaxy types. Methods. We studied the evolution in the B band LF to redshift z ~ 1 in the zCOSMOS 10k sample, for which both accurate galaxy classifications (spectrophotometric and morphological) and a detailed description of the local density field are available. Results. The global B band LF exhibits a brightening of ~0.7 mag in M^* from z ~ 0.2 to z ~ 0.9. At low redshifts (z<0.35), spectrophotometric late types dominate at faint magnitudes (M_B_(AB) > -20), while the bright end is populated mainly by spectrophotometric early types. At higher redshift, spectrophotometric late-type galaxies evolve significantly and, at redshift z ~ 1, the contribution from the various types to the bright end of the LF is comparable. The evolution for spectrophotometric early-type galaxies is in both luminosity and normalization: M* brightens by ~0.6 mag but φ^∗ decreases by a factor ~1.7 between the first and the last redshift bin. A similar behaviour is exhibited by spectrophotometric late-type galaxies, but with an opposite trend for the normalization: a brightening of ~0.5 mag is present in M^*, while φ^∗ increases by a factor ~1.8.
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. These results indicate that galaxies of the same type in different environments have different properties.
We also detect a differential evolution in blue galaxies in different environments: the evolution in their LF is similar in underdense and overdense regions between z ~ 0.25 and z ~ 0.55, and is mainly in luminosity. In contrast, between z ~ 0.55 and z ~ 0.85 there is little luminosity evolution but there is significant evolution in φ^∗, that is, however, different between the two environments: in overdense regions φ^∗ increases by a factor ~1.6, while in underdense regions this increase reaches a factor ~2.8. Analyzing the blue galaxy population in more detail, we find that this evolution is driven mainly by the bluest types. Conclusions. 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 redshifts in underdense environments.

Item Type:Article
Related URLs:
URLURL TypeDescription
Ilbert, O.0000-0002-7303-4397
Lilly, S.0000-0002-6423-3597
Caputi, K.0000-0001-8183-1460
Carollo, C. M.0000-0003-1624-7609
Kneib, J.-P.0000-0002-4616-4989
Le Fèvre, O.0000-0001-5891-2596
Renzini, A.0000-0002-7093-7355
Cucciati, O.0000-0002-9336-7551
de la Torre, S.0000-0002-0839-2884
Silverman, J. D.0000-0002-0000-6977
Tanaka, M.0000-0002-5011-5178
Koekemoer, A. M.0000-0002-6610-2048
Leauthaud, A.0000-0002-3677-3617
McCracken, H. J.0000-0002-9489-7765
Oesch, P.0000-0001-5851-6649
Aussel, H.0000-0002-1371-5705
Capak, P.0000-0003-3578-6843
Kartaltepe, J.0000-0001-9187-3605
Salvato, M.0000-0001-7116-9303
Sanders, D.0000-0002-1233-9998
Scoville, N.0000-0002-0438-3323
Taniguchi, Y.0000-0003-2247-3741
Additional Information:© 2009 ESO. Received 9 June 2009; accepted 17 September 2009. We acknowledge support from an INAF contract PRIN- 2007/ and an ASI grant ASI/COFIS/WP3110 I/026/07/0.
Group:COSMOS, Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Istituto Nazionale di Astrofisica (INAF)PRIN-2007/
Agenzia Spaziale Italiana (ASI)ASI/COFIS/WP3110 I/026/07/0
Subject Keywords:galaxies: evolution; galaxies: luminosity function, mass function; galaxies: statistics; Surveys
Issue or Number:3
Record Number:CaltechAUTHORS:20100113-153659302
Persistent URL:
Official Citation:The zCOSMOS survey: the role of the environment in the evolution of the luminosity function of different galaxy types E. Zucca, S. Bardelli, M. Bolzonella, G. Zamorani, O. Ilbert, L. Pozzetti, M. Mignoli, K. Kova, S. Lilly, L. Tresse, L. Tasca, P. Cassata, C. Halliday, D. Vergani, K. Caputi, C. M. Carollo, T. Contini, J.-P. Kneib, O. Le Fèvre, V. Mainieri, A. Renzini, M. Scodeggio, A. Bongiorno, G. Coppa, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, C. Knobel, F. Lamareille, J.-F. Le Borgne, V. Le Brun, C. Maier, R. Pellò, Y. Peng, E. Perez-Montero, E. Ricciardelli, J. D. Silverman, M. Tanaka, U. Abbas, D. Bottini, A. Cappi, A. Cimatti, L. Guzzo, A. M. Koekemoer, A. Leauthaud, D. Maccagni, C. Marinoni, H. J. McCracken, P. Memeo, B. Meneux, M. Moresco, P. Oesch, C. Porciani, R. Scaramella, S. Arnouts, H. Aussel, P. Capak, J. Kartaltepe, M. Salvato, D. Sanders, N. Scoville, Y. Taniguchi and D. Thompson A&A 508 (3) 1217-1234 (2009) DOI: 10.1051/0004-6361/200912665
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:17171
Deposited On:14 Jan 2010 21:38
Last Modified:08 Nov 2021 23:33

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