Issue |
A&A
Volume 508, Number 3, December IV 2009
|
|
---|---|---|
Page(s) | 1217 - 1234 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/200912665 | |
Published online | 01 October 2009 |
The zCOSMOS survey: the role of the environment in the evolution of the luminosity function of different galaxy types*
1
INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: elena.zucca@oabo.inaf.it
2
Laboratoire d'Astrophysique de Marseille, Université d'Aix-Marseille, CNRS, 38 rue Frederic Joliot-Curie, 13388 Marseille Cedex 13, France
3
Institute of Astronomy, Swiss Federal Institute of Technology (ETH Hönggerberg), 8093 Zürich, Switzerland
4
INAF - IASF Milano, via Bassini 15, 20133 Milano, Italy
5
Department of Astronomy, University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01003, USA
6
INAF - Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy
7
Laboratoire d'Astrophysique de Toulouse-Tarbes, Université de Toulouse, CNRS, 14 avenue Edouard Belin, 31400 Toulouse, France
8
European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
9
INAF - Osservatorio Astronomico di Padova, vicolo Osservatorio 5, 35122 Padova, Italy
10
Max-Planck-Institut für extraterrestrische Physik, 84571 Garching, Germany
11
Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy
12
INAF - Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy
13
Instituto de Astrofisica de Andalucia, CSIC, Apdo. 3004, 18080 Granada, Spain
14
Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio 3, 35122 Padova, Italy
15
INAF - Osservatorio Astronomico di Torino, strada Osservatorio 20, 10025 Pino Torinese, Italy
16
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MS 21218, USA
17
LBNL & BCCP, University of California, Berkeley, CA 94720, USA
18
Centre de Physique Theorique, Marseille, France
19
Institut d'Astrophysique de Paris, UMR 7095 CNRS, Université Pierre et Marie Curie, 98 bis Boulevard Arago, 75014 Paris, France
20
Universitäts-Sternwarte, Scheinerstrasse 1, 81679 Munich, Germany
21
Argelander-Institut für Astronomie, Auf dem Hügel 71, 53121 Bonn, Germany
22
INAF, Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monteporzio Catone, Italy
23
Canada-France-Hawaii Telescope Corporation, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USA
24
AIM Unité Mixte de Recherche CEA CNRS, Université Paris VII UMR 158, Paris, France
25
California Institute of Technology, MC 105-24, 1200 East California Boulevard, Pasadena, CA 91125, USA
26
Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI, 96822, USA
27
Research Center for Space and Cosmic Evolution, Ehime University, Bunkyo-cho, Matsuyama 790-8577, Japan
28
Large Binocular Telescope Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721-0065, USA
Received:
9
June
2009
Accepted:
17
September
2009
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 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 to
.
At low redshifts (
), spectrophotometric late types dominate at
faint magnitudes (
), while the bright end is populated
mainly by spectrophotometric early types.
At higher redshift, spectrophotometric late-type galaxies evolve significantly and, at
redshift
,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
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
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
and
, and is mainly in luminosity.
In contrast, between
and
there is little luminosity evolution but there is significant
evolution in
, that is, however, different between the two environments:
in overdense regions
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 , while it is still ongoing at lower
redshifts in underdense environments.
Key words: galaxies: evolution / galaxies: luminosity function, mass function / galaxies: statistics / Surveys
© ESO, 2009
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