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The <i>XMM‐Newton</i> Wide‐Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies

A. FinoguenovMax-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, GermanyL. GuzzoOsservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate, ItalyG. HasingerMax-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, GermanyN. Z. ScovilleCalifornia Institute of Technology, MC 105-24, 1200 East California Boulevard, Pasadena, CA 91125H. AusselService d’Astrophysique, CEA/Saclay, 91191 Gif-sur-Yvette, FranceH. BöhringerMax-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, GermanyM. BrusaMax-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, GermanyP. CapakCalifornia Institute of Technology, MC 105-24, 1200 East California Boulevard, Pasadena, CA 91125N. CappellutiMax-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, GermanyA. ComastriINAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, ItalyS. GiodiniOsservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate, ItalyR. E. GriffithsDepartment of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213C. ImpeySteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721A. M. KoekemoerSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218Jean‐Paul KneibLaboratoire d’Astrophysique de Marseille, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, FranceA. LeauthaudLaboratoire d’Astrophysique de Marseille, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, FranceO. Le FèvreLaboratoire d’Astrophysique de Marseille, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, FranceS. J. LillyDepartment of Physics, Eidgenössische Technische Hochschule-Zurich, CH-8093 Zurich, SwitzerlandV. MainieriEuropean Southern Observatory, Karl-Schwarzschild-Strasse 2, Garching D-85748, GermanyR. MasseyCalifornia Institute of Technology, MC 105-24, 1200 East California Boulevard, Pasadena, CA 91125H. J. McCrackenInstitut d’Astrophysique de Paris, UMR7095 CNRS, Universitè Pierre et Marie Curie, 98 bis Boulevard Arago, 75014 Paris, FranceB. MobasherSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218Takashi MurayamaAstronomical Institute, Graduate School of Science, Tohoku University, Aramaki, Aoba, Sendai 980-8578, JapanJ. A. PeacockInstitute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UKI. SakelliouMax-Planck-Institut für Astronomie, Königstuhl 17, Heidelberg D-69117, GermanyEva SchinnererMax-Planck-Institut für Astronomie, Königstuhl 17, Heidelberg D-69117, GermanyJ. D. SilvermanMax-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, GermanyV. SmolčićMax-Planck-Institut für Astronomie, Königstuhl 17, Heidelberg D-69117, GermanyYuki TaniguchiPhysics Department, Graduate School of Science, Ehime University, 2-5 Bunkyou, Matuyama, 790-8577, JapanL. TascaLaboratoire d’Astrophysique de Marseille, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, FranceJames E. TaylorCalifornia Institute of Technology, MC 105-24, 1200 East California Boulevard, Pasadena, CA 91125Jonathan R. TrumpSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721G. ZamoraniINAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy

2007en

ABI

Annotatsiya

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.\n

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DOI: 10.1086/516577

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