Issue |
A&A
Volume 504, Number 2, September III 2009
|
|
---|---|---|
Page(s) | 331 - 346 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361/200809964 | |
Published online | 15 July 2009 |
GMASS ultradeep spectroscopy of galaxies at z ~ 2 *,**
V. Witnessing the assembly at z = 1.6 of a galaxy cluster
1
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: kurk@mpia.de
2
INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
3
Università di Bologna, Dipartimento di Astronomia, via Ranzani 1, 40127 Bologna, Italy
4
INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
5
CEA, Laboratoire AIM - CNRS - Université Paris Diderot, Irfu/SAp, Orme des Merisiers, 91191 Gif-sur-Yvette, France
6
European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
7
NOAO-Tucson, 950 North Cherry Avenue, Tucson, AZ 85719, USA
8
Department of Astronomy, University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01003, USA
9
INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy
10
Università di Padova, Dipartimento di Astronomia, Vicolo dell'Osservatorio 2, 35122 Padova, Italy
11
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85748 Garching bei München, Germany
Received:
14
April
2008
Accepted:
10
June
2009
Context. Clusters of galaxies represent important laboratories for studying
galaxy evolution and formation. Well established and relaxed
clusters are known below , as well as, clusters in
formation found close to radio galaxies at
, but the
in-between redshift range, during which clusters are expected to
undergo significant changes, is almost unexplored.
Aims. By studying a galaxy overdensity in redshift and angular
distribution at , uncovered in the Galaxy Mass Assembly
ultra-deep Spectroscopic Survey (GMASS), we provide insight into the
evolution of cluster galaxies at high redshift.
Methods. We present a study of the significance of the galaxy overdensity at
, Cl 0332-2742, its velocity dispersion, and X-ray emission.
We identify the colour bimodality of the cluster members and compare the
properties of members of Cl 0332-2742 with galaxies outside the
overdensity.
Results. From the redshifts of the 42 overdensity members, we measure a velocity
dispersion of 500 km s-1. We conservatively estimate the
overdensity in redshift space for the spike at in the GMASS field
to be
. A map of the surface density of galaxies at
in the GMASS field shows that its structure is irregular
with several filaments and local overdensities. The differences in
the physical properties of Cl 0332-2742 member and field galaxies agree with
the latest hierarchical galaxy formation models: for overdensity
members, the star formation rate (
), and specific
, is
approximately 50% lower than for the field galaxies; overdensity
galaxies are twice the age, on average, of field galaxies; and there
is a higher proportion of both massive (
), and
early-type galaxies, inside Cl 0332-2742 than in the field. Among the
42 members, seven have spectra consistent with being passively evolving,
massive galaxies. These are all located within an area where the
surface density of
galaxies is highest. In a
colour–magnitude diagram, the photometric data of these early-type
galaxies are in close agreement with a theoretical red sequence of a
galaxy cluster at redshift
, which formed most of its stars
in a short burst of star formation at
.
Conclusions. We conclude that the redshift spike at in the GMASS
field represents a sheet-like structure in the cosmic web, and that the
area with the highest surface density within this structure,
containing already seven passively evolving galaxies, will evolve
into a cluster of galaxies at a later time.
Key words: galaxies: distances and redshifts / galaxies: evolution / galaxies: formation / galaxies: clusters: general / galaxies: high-redshift
© ESO, 2009
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