Issue |
A&A
Volume 439, Number 3, September I 2005
|
|
---|---|---|
Page(s) | 877 - 885 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20041962 | |
Published online | 12 August 2005 |
The VIMOS VLT deep survey
The evolution of galaxy clustering to z
2 from first
epoch observations
1
Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, Traverse du Siphon, BP 8, 13012 Marseille, France e-mail: olivier.lefevre@oamp.fr
2
INAF – Osservatorio Astronomico di Brera, via Brera 28, 20121 Milan, Italy
3
INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
4
Institut d'Astrophysique de Paris, UMR 7095, 98bis Bd. Arago, 75014 Paris, France
5
Observatoire de Paris, LERMA, UMR 8112, 61 Av. de l'Observatoire, 75014 Paris, France
6
INAF – Osservatorio Astronomico di Roma, Italy
7
INAF – IASF, via Bassini, 15, 20133 Milano, Italy
8
Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées, UMR 5572, 14 Av. Ed. Belin, 31400 Toulouse, France
9
INAF – Istituto di Radio-Astronomia, via Gobetti 101, 40129 Bologna, Italy
10
INAF – Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy
11
Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy
12
Max-Planck-Institut für Astrophysik, 85741 Garching, Germany
13
European Southern Observatory, Karl Schwarzschild Str. 2, 85748 Garching bei München, Germany
Received:
6
September
2004
Accepted:
11
April
2005
This paper presents the evolution of the
clustering of the main population of
galaxies from to
, from the first epoch
VIMOS VLT Deep Survey (VVDS), a magnitude limited sample with
.
The sample allows a direct estimate of evolution from within the same survey over the time base sampled.
We have computed the correlation functions
and
,
and the correlation length
,
for the VVDS-02h and VVDS-CDFS fields, for a total of 7155 galaxies in a
0.61 deg2 area. We find that the correlation length
in this sample slightly increases from
to
,
with
h-1 Mpc (comoving), for galaxies
comparable in luminosity to the local 2dFGRS
and SDSS samples,
indicating that the amplitude of the correlation function
was
2.5 times lower at
than observed
locally. The correlation length in our lowest redshift bin
is
h-1 Mpc, lower than for any other population at
the same redshift, indicating the low clustering of
very low luminosity galaxies, 1.5 mag fainter than in the
2dFGRS or SDSS. The correlation length
increases to
h-1 Mpc at higher redshifts
,
as we are observing increasingly brighter galaxies, comparable
to galaxies with
locally.
We compare our measurement to the DEEP2 measurements in
the range
(Coil et al. 2004, ApJ, in press) and find comparable results
when applying the same magnitude and color selection
criteria as in their survey.
The slowly varying clustering of VVDS galaxies as redshift increases
is markedly different from the predicted evolution
of the clustering of dark matter,
indicating that bright galaxies traced higher density
peaks when the large scale structures were emerging from the
dark matter distribution 9–10 billion years ago,
being supporting evidence for a strong evolution of the
galaxy vs. dark matter bias.
Key words: surveys / galaxies: evolution / cosmology: large scale structure of Universe
© ESO, 2005
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