Issue |
A&A
Volume 442, Number 3, November II 2005
|
|
---|---|---|
Page(s) | 801 - 825 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20052966 | |
Published online | 14 October 2005 |
The VIMOS VLT Deep Survey
Evolution of the non-linear galaxy bias up to z = 1.5
1
INAF - Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italia
2
Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS-Université de Provence, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France e-mail: christian.marinoni@cpt.univ-mrs.fr
3
INAF - Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate, Italia
4
INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italia
5
INAF - Osservatorio Astronomico di Roma, via Osservatorio 2, 00040 Monteporzio Catone (Roma), Italia
6
Institut d'Astrophysique de Paris, UMR 7095, 98 bis Bd Arago, 75014 Paris, France
7
INAF - IASF, Via Bassini 15, 20133 Milano, Italia
8
Laboratoire d'Astrophysique - Observatoire Midi-Pyrénées, Toulouse, France
9
INAF - Istituto di Radio-Astronomia, Via Gobetti 101, 40129 Bologna, Italia
10
Università di Bologna, Dipartimento di Astronomia, via Ranzani 1, 40127 Bologna, Italia
11
Max Planck Institut fur Astrophysik, 85741 Garching, Germany
12
INAF - Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italia
13
Università di Milano-Bicocca, Dipartimento di Fisica, Piazza della scienza 3, 20126 Milano, Italia
Received:
2
March
2005
Accepted:
17
June
2005
We present the first measurements of the Probability
Distribution Function (PDF) of galaxy fluctuations in the four-passes,
first-epoch VIMOS-VLT Deep Survey (VVDS) cone, covering
deg between
. We show that the PDF
of density contrasts of the VVDS galaxies is an unbiased tracer of the underlying
parent distribution up to redshift z=1.5, on scales R=8 and
10 h-1Mpc. The second moment of the PDF, i.e. the rms fluctuations
of the galaxy density field, is to a good approximation constant over the
full redshift baseline investigated: we find that, in redshift space,
for galaxies brighter than
has a mean value of
in the redshift interval
. The third moment, i.e. the skewness,
increases with cosmic time: we find that the probability of having
underdense regions is greater at
than it was at
. By comparing the PDF of galaxy density contrasts with the
theoretically predicted PDF of mass fluctuations we infer the
redshift-, density- and scale-dependence of the biasing function
between galaxy and matter overdensities up to redshift
z=1.5. Our results can be summarized as follows:
i) the galaxy bias is an increasing function of redshift:
evolution is marginal up to
and more pronounced
for
;
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 >5 h-1Mpc. By subdividing the
sample according to galaxy luminosity and colors, we also show that:
iv) brighter galaxies are more strongly biased than less luminous
ones at every redshift and the dependence of biasing on luminosity at
is in good agreement with what is observed in the local
Universe; v) red objects are systematically more biased than blue
objects at all cosmic epochs investigated, but
the relative bias between red and blue
objects is constant as a function of redshift in the interval
,
and its value (
) is similar to what is found at
.
Key words: cosmology: large-scale structure of Universe / galaxies: distances and redshifts / galaxies: evolution / galaxies: statistics
© ESO, 2005
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