Issue |
A&A
Volume 442, Number 3, November II 2005
|
|
---|---|---|
Page(s) | 841 - 849 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20053433 | |
Published online | 14 October 2005 |
New spectroscopic confirmations of high-redshift galaxy clusters
1
Observatoire de la Côte d'Azur, Laboratoire Cassiopée, BP 4229, 06304 Nice Cedex 4, France
2
Niels Bohr Institute, Copenhagen University, Juliane Maries Vej 30, 2100 Copenhagen, Denmark e-mail: lisbeth@astro.ku.dk
3
INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
4
Observatorio Nacional, Rua General Jose Cristinino 77, CEP 20921-400, Rio de Janeiro JR, Brazil
5
European Southern Observatory, Karl-Schwartzschild-Str. 2, 85748 Garching b. München, Germany
6
INAF - Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, 34131 Trieste, Italy
Received:
13
May
2005
Accepted:
21
July
2005
We present new spectroscopic data in the field of five
high-redshift () candidate galaxy clusters, drawn from
the EIS Cluster Candidate Catalog. A total of 327 spectra were
obtained using FORS1 at the VLT, out of which 266 are galaxies with
secure redshifts. In this paper, we use these data for confirming
the existence of overdensities in redshift space at the approximate
same location as the matched-filter detections in the projected
distribution of galaxies from the EIS I-band imaging survey. The
spectroscopic redshifts, associated to these overdensities, are
consistent but, in general, somewhat lower than those predicted by
the matched-filter technique. Combining the systems presented here
with those analyzed earlier, we have spectroscopically confirmed a
total of nine overdensities in the redshift range
,
providing an important first step in building an
optically-selected, high-redshift sample for more detailed studies,
complementing those based on the few available X-ray selected
systems.
Key words: cosmology: observations / galaxies: distances and redshifts / galaxies: clusters: general
© ESO, 2005
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