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

By A. Finoguenov, L. Guzzo, G. Hasinger, N. Scoville, N. Scoville, H. Aussel, H. Böhringer, M. Brusa, P. Capak, N. Cappelluti and 24 more. 2006

236 citations recorded by the source corpus.

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)- 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 × 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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/711eb2a63ae73239778e5170c6ee28a545334f1b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Tracking the impact of environment on the galaxy stellar mass function up to z ~ 1 in the 10 k zCOSMOS sample (2009, background): “…high density environments in which galaxies reside can be obtained by selecting optical groups, as described in Knobel et al. (2009), or X-ray ones (Finoguenov et al. 2007; Finoguenov et al. 2009); low density environments can be tracked by isolated galaxies defined using their Voronoi volumes, as…”
EVOLUTION OF GALAXIES AND THEIR ENVIRONMENTS AT z = 0.1–3 IN COSMOS (2013, methodology): “…lensing tomography and hot X-ray emitting gas in the virialized clusters/groups of galaxies at z < 1.1 (Scoville et al. 2007b; Massey et al. 2007; Finoguenov et al. 2007); here we extend this investigation to higher z and lower density LSS using deeper photometry and high accuracy photometric…”
The XMM Cluster Survey:Optical analysis methodology and the first data release (2011, background): “2+024137.4 (z = 0.35; Finoguenov et al. 2007), which was detected near the XMM aim-point, but was still a genuine serendipitous detection because that ObsID was part of a blind survey towards the COSMOS field (Scoville et al. 2007).”
The galaxy luminosity function at z ≃ 6 and evidence for rapid evolution in the bright end from z ≃ 7 to 5 (2014, methodology): “The UltraVISTA/COSMOS and UDS/SXDS fields have been observed to similar depths (' 2–3×10−15 ergs cm−2s−1 at 0.5–2 keV) with XMM-Newton, and the X-ray bright clusters have been identified by Finoguenov et al. (2007) and Finoguenov et al. (2010) in each field respectively.”
The XMM-Newton Wide-Field Survey in the COSMOS Field. III. Optical Identification and Multiwavelength Properties of a Large Sample of X-Ray-Selected Sources (2006, background): “The X–ray point source counts from the first 800 ks of the XMM–Newton observations obtained so far are presented in Cappelluti et al. (2007), while the properties of extended and diffuse sources are described in Finoguenov et al. (2007).”
THE RISE AND FALL OF PASSIVE DISK GALAXIES: MORPHOLOGICAL EVOLUTION ALONG THE RED SEQUENCE REVEALED BY COSMOS (2009, background): “These were identified in the X-ray-selected COSMOS group catalog assembled by Finoguenov et al. (2007) and Leauthaud et al. (2010) which contains 206 groups with weak-lensing calibrated virial (total) masses complete to M200 ≈ 3× 1013M to z = 0.5 and M200 ≈ 3× 1014M to z = 1.0.”
The WIRCam Deep Survey I. Counts, colours, and mass-functions derived from near-infrared imaging in the CFHTLS deep fields (2011, background): “Furthermore, deep, wide, near-infrared data facilitates the identification of high-redshift groups and clusters (e.g. Finoguenov et al. 2007; Bielby et al. 2010; Finoguenov et al. 2010; Henry et al. 2010; Gobat et al. 2011; Fassbender et al. 2011) and the first populations of galaxies in the early…”
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION (2009, methodology): “…et al. 2002; Benson et al. 2004; Staniszewski et al. 2008), c) detection via X-ray emission (e.g. Böhringer et al. 2000; Hasinger et al. 2001; Finoguenov et al. 2007; Vikhlinin et al. 2008), d) spectroscopic identification (e.g. Gerke et al. 2005; Miller et al. 2005; Knobel et al. 2009),…”
THE CHANDRA COSMOS LEGACY SURVEY: OVERVIEW AND POINT SOURCE CATALOG (2016, methodology): “To avoid contamination by extended sources, we used the XMM-COSMOS catalog of extended sources (Finoguenov et al. 2007, Kettula et al. 2013) and visually inspected all the brightest (LX > 10 41 erg s−1 in 0.5-2 keV) ones to check if a point source is detected inside them by Chandra.”
PHOTOMETRIC REDSHIFT AND CLASSIFICATION FOR THE XMM–COSMOS SOURCES (2008, background): “The redshift distribution shows significant peaks at z∼0.35, ∼0.8, corresponding to spectroscopically confirmed galaxy over-densities in the COSMOS field (Scoville et al. 2007a; Finoguenov et al. 2007; Lilly et al. 2007; Gilli et al. 2008).”
Photometric Redshifts of Galaxies in COSMOS (2006, methodology): “These results are used to identify the large-scale structures (Scoville et al. 2007; Finoguenov et al. 2007; Guzzo et al. 2007), to study the evolution of density-morphology relation (Capak et al. 2007a), to study dependence of the star formation activity on the environment (Mobasher et al. 2007)…”
STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, methodology): “The X-ray data reduction is described in detail in Finoguenov et al. (2007) and Finoguenov et al. (in preparation).”
SPECTROSCOPIC CONFIRMATION OF TWO MASSIVE RED-SEQUENCE-SELECTED GALAXY CLUSTERS AT z ∼ 1.2 IN THE SpARCS-NORTH CLUSTER SURVEY (2008, methodology): “2 The largest area targeted X-ray cluster surveys are the XMM-LSS (Valtchanov et al. 2004; Andreon et al. 2005; Pierre et al. 2006) and the XMM-COSMOS (Finoguenov et al. 2007), and while these have been successful at discovering z > 1 clusters (e.g., Bremer et al. 2006), they cover areas of only 9 a”
The dependence of star formation activity on environment and stellar mass at z∼ 1 from the HiZELS-Hα survey (2010, background): “…the survey is able to probe a luminous and massive (M500 ≈ 1014.3 M ) X-ray selected cluster in COSMOS at z = 0.835 (see Figure 2), along with other nearby lower luminosity X-ray groups at z = 0.85 which have already been reported by the COSMOS team (Finoguenov et al. 2007; Leauthaud et al. 2010).”