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J/ApJS/172/182    XMM Clusters of galaxies in COSMOS field   (Finoguenov+ 2007)

The XMM-Newton wide-field survey in the COSMOS field: statistical properties of clusters of galaxies. Finoguenov A., Guzzo L., Hasinger G., Scoville N.Z., Aussel H., Bohringer H., Brusa M., Capak P., Cappelluti N., Comastri A., Giodini S., Griffiths R.E., Impey C., Koekemoer A.M., Kneib J.-P., Leauthaud A., Le Fevre O., Lilly S., Mainieri V., Massey R., McCracken H.J., Mobasher B., Murayama T., Peacock J.A., Sakelliou I., Schinnerer E., Silverman J.D., Smolcic V., Taniguchi Y., Tasca L., Taylor J.E., Trump J.R., Zamorani G. <Astrophys. J. Suppl. Ser., 172, 182-195 (2007)> =2007ApJS..172..182F
ADC_Keywords: Surveys ; X-ray sources ; Clusters, galaxy Keywords: cosmology: observations - dark matter - large-scale structure of universe - surveys 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 0.5-2keV band of 3x10-15ergs/cm2/s, having one of the widest XMM-Newton contiguous raster surveys, covering an area of 2.1deg2. 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 alpha=1.93±0.04. For the probed luminosity range of (8x1042)-(2x1044)ergs/s, 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. Description: For cluster detection, we used the XMM-Newton mosaic image in the 0.5-2keV band, based on the first 36 pointings of the XMM-Newton observations of the COSMOS field. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 75 72 Catalog of the identified X-ray clusters
See also: B/xmm : XMM-Newton Observation Log (XMM-Newton SOC, 2007) II/284 : COSMOS Multi-Wavelength Photometry Catalog (Capak+, 2007) J/ApJS/172/29 : XMM-Newton survey in COSMOS field. I. (Hasinger+, 2007) J/ApJS/172/368 : XMM-Newton survey in COSMOS field. IV. (Mainieri+, 2007) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- [FGH2007] Sequential number 5- 13 F9.5 deg RAdeg Right ascension in decimal degrees (J2000.0) 15- 21 F7.5 deg DEdeg Declination in decimal degrees (J2000.0) 23- 25 F3.1 arcmin r500 Estimated radius 27- 31 F5.2 10-17W/m2 Flux Cluster flux on the 0.5-2keV 33- 36 F4.2 10-17W/m2 e_Flux rms uncertainty on Flux 38- 41 F4.2 --- z Photometric redshift 43- 47 F5.2 10+13solMass M500 Estimated cluster mass 49- 52 F4.2 10+13solMass e_M500 rms uncertainty on M500 54- 58 F5.1 10+35W Lum 0.1-2.4keV luminosity 60- 63 F4.1 10+35W e_Lum 0.1-2.4keV luminosity 65- 68 F4.2 keV kT IGM temperature 70- 73 F4.2 keV e_kT rms uncertainty on kT 75 I1 --- r_z [0/1] Redshift reference (1)
Note (1): Redshift reference as follows: 0 = redshift from SDSS DR4 1 = redshift estimate
History: From electronic version of the journal References: Hasinger et al., Paper I 2007ApJS..172...29H, Cat. J/ApJS/172/29 Cappelluti et al., Paper II 2007ApJS..172..341C Brusa et al., Paper III 2007ApJS..172..353B Mainieri et al., Paper IV 2007ApJS..172..368M, Cat. J/ApJS/172/368 Miyaji et al., Paper V 2007ApJS..172..396M
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 04-Mar-2008
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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