Volume 503, Number 2, August IV 2009
|Page(s)||399 - 408|
|Section||Cosmology (including clusters of galaxies)|
|Published online||09 July 2009|
Cluster and cluster galaxy evolution history from IR to X-ray observations of the young cluster RX J1257.2+4738 at z = 0.866*
LAM, Pôle de l'Etoile Site Château-Gombert, 38 rue Frédéric Juliot-Curie, 13388 Marseille Cedex 13, France e-mail: email@example.com
2 Department of Physics and Astronomy, Northwestern University, 2131 Sheridan Road, Evanston IL 60208-2900, USA
3 Instituto de Astronomia, Geofísica e C. Atmosf./USP, R. do Matão 1226, 05508-090 São Paulo/SP, Brazil
4 Institut d'Astrophysique de Paris, CNRS, UMR 7095, Université Pierre et Marie Curie, 98bis Bd Arago, 75014 Paris, France
5 Università di Napolia “Federico II”, Dipartimento di Sciennze Fisiche and INAF – Observatorio Astronomico di Capodimonte, v. Moiariello 16, 80131 Napoli, Italy
6 Institute for Astronomy, 2680 Woodlawn Dr., University of Hawaii, Honolulu, Hawaii 96822, USA
7 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
8 Fermi National Accelerator Laboratory, MS 127, PO Box 500, Batavia, IL 60510, USA
9 University of Chicago, Department of Astronomy and Astrophysics, 5640 South Ellis Avenue, Chicago, IL 60637, USA
10 California Institute of Technology, Spitzer Science Center, MS 314-6, 1200 East California Blvd, Pasadena, CA 91125, USA
Accepted: 30 June 2009
Context. The cosmic time around the z ~ 1 redshift range appears crucial in the cluster and galaxy evolution, since it is probably the epoch of the first mature galaxy clusters. Our knowledge of the properties of the galaxy populations in these clusters is limited because only a handful of z ~ 1 clusters are presently known.
Aims. In this framework, we report the discovery of a z ~ 0.87 cluster and study its properties at various wavelengths.
Methods. We gathered X-ray and optical data (imaging and spectroscopy), and near and far infrared data (imaging) in order to confirm the cluster nature of our candidate, to determine its dynamical state, and to give insight on its galaxy population evolution.
Results. Our candidate structure appears to be a massive z ~ 0.87 dynamically young cluster with an atypically high X-ray temperature as compared to its X-ray luminosity. It exhibits a significant percentage (~90%) of galaxies that are also detected in the 24 μm band.
Conclusions. The cluster RXJ1257.2+4738 appears to be still in the process of collapsing. Its relatively high temperature is probably the consequence of significant energy input into the intracluster medium besides the regular gravitational infall contribution. A significant part of its galaxies are red objects that are probably dusty with on-going star formation.
Key words: galaxies: clusters: individual: RX J1257.2+4738 / galaxies: clusters: general / Galaxy: evolution
Partly based on observations with Chandra which is operated by the Harvard-Smithsonian Center for Astrophysics under contract with NASA. Partly based on observations obtained at the Gemini Observatory which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil) and SECYT (Argentina). Partly based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Partly based on observations obtained with the Apache Point Observatory 3.5-m telescope, which is owned and operated by the Astrophysical Research Consortium (ARC). Partly based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Partly based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). Partly based on observations obtained at the Observatoire de Haute Provence (CNRS) with the 1.93-m telescope and the CARELEC instrument.
© ESO, 2009
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