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Published September 2007 | Published
Journal Article Open

The XMM-Newton Wide-Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies


We present the results of a search for galaxy clusters in the first 36 XMM-Newton pointings on the Cosmic Evolution Survey (COSMOS) field. We reach a depth for a total cluster flux in the 0.5-2 keV band of 3 × 10^(-15) ergs cm^(-2) s^(-1), having one of the widest XMM-Newton contiguous raster surveys, covering an area of 2.1 deg^2. Cluster candidates are identified through a wavelet detection of extended X-ray emission. Verification of the cluster candidates is done based on a galaxy concentration analysis in redshift slices of thickness 0.1-0.2 in redshift, using the multiband photometric catalog of the COSMOS field and restricting the search to z < 1.3 and i_(AB) < 25. We identify 72 clusters and derive their properties based on the X-ray cluster scaling relations. A statistical description of the survey in terms of the cumulative log(N > S)-log S distribution compares well with previous results, although yielding a somewhat higher number of clusters at similar fluxes. The X-ray luminosity function of COSMOS clusters matches well the results of nearby surveys, providing a comparably tight constraint on the faint-end slope of α = 1.93 ± 0.04. For the probed luminosity range of (8 × 10^(42))-(2 × 10^(44)) ergs s^(-1), our survey is in agreement with and adds significantly to the existing data on the cluster luminosity function at high redshifts and implies no substantial evolution at these luminosities to z = 1.3.

Additional Information

© 2007 American Astronomical Society. Received 2006 April 24; accepted for publication 2006 November 23. This research is based on observations with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; and the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS5-26555; it is also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter- American Observatory, and the National Optical Astronomy Observatory, which are operated by AURA, Inc., under cooperative agreement with the National Science Foundation (NSF); the National Radio Astronomy Observatory, which is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc.; and the Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii. In Germany, the XMM-Newton project is supported by the Bundesministerium fuer Wirtschaft und Technologie/Deutsches Zentrum fuer Luft-und Raumfahrt (BMWI/DLR, FKZ 50 OX 0001), the Max Planck Society, and the Heidenhain-Stiftung. Part of this work was supported by the Deutsches Zentrum fu¨ r Luft-und Raumfahrt, DLR project numbers 50 OR 0207 and 50 OR 0405. The HST COSMOS Treasury program was supported through NASA grant HST-GO- 09822.We gratefully acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 70 scientists. More information on the COSMOS survey is available at http:// www.astro.caltech.edu/cosmos. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. The COSMOS Science meeting in 2005 May was supported in part by the NSF through grant OISE- 0456439. A. F. acknowledges support from BMBF/DLR under grant 50 OR 0207, MPG, and a partial support from NASA grant NNG04GF686, covering his stays at UMBC. The authors thank the referee, Alastair Edge, for detailed comments, which improved the content of this paper. A. F. thanks Harald Ebeling, Trevor Ponman, Piero Rosati, and Peter Schuecker for useful suggestions at various stages of this work. I. S. acknowledges the support of the European Community under a Marie Curie Intra-European Fellowship.

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