The XMM-Newton Wide-Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies
Finoguenov, A.; Böhringer, H.; Kneib, J. -P.; Aussel, H.; Murayama, T.; Smolčić, V.; Taniguchi, Y.; Silverman, J. D.; Comastri, A.; Cappelluti, N.; Brusa, M.; Hasinger, G.; Mainieri, V.; Capak, P.; Koekemoer, A. M.; Schinnerer, E.; Scoville, N. Z.; Lilly, S.; McCracken, H. J.; Zamorani, G.; Tasca, L.; Le Fèvre, O.; Impey, C.; Mobasher, B.; Massey, R.; Griffiths, R. E.; Trump, J. R.; Leauthaud, A.; Peacock, J. A.; Taylor, J. E.; Guzzo, L.; Sakelliou, I.; Giodini, S.
Germany, United States, Italy, France, Switzerland, Japan, United Kingdom
Abstract
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 deg2. 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 iAB<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)-logS 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 (8×1042)-(2×1044) 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.