Mon. Not. R. Astron. Soc., 372, 591-608 (2006/October-3)
The XMM Large-Scale Structure survey: a well-controlled X-ray cluster sample over the D1 CFHTLS area.
PIERRE M., PACAUD F., DUC P.-A., WILLIS J.P., ANDREON S., VALTCHANOV I., ALTIERI B., GALAZ G., GUEGUEN A., LE FEVRE J.-P., LE FEVRE O., PONMAN T., SPRIMONT P.-G., SURDEJ J., ADAMI C., ALSHINO A., BREMER M., CHIAPPETTI L., DETAL A., GARCET O., GOSSET E., JEAN C., MACCAGNI D., MARINONI C., MAZURE A., QUINTANA H. and READ A.
Abstract (from CDS):
We present the XMM Large-Scale Structure Survey (XMM-LSS) cluster catalogue corresponding to the Canada-France-Hawaii Telescope Legacy Survey D1 area. The list contains 13 spectroscopically confirmed, X-ray selected galaxy clusters over 0.8deg2 to a redshift of unity and so constitutes the highest density sample of clusters to date. Cluster X-ray bolometric luminosities range from 0.03 to 5x1044erg/s. In this study, we describe our catalogue construction procedure: from the detection of X-ray cluster candidates to the compilation of a spectroscopically confirmed cluster sample with an explicit selection function. The procedure further provides basic X-ray products such as cluster temperature, flux and luminosity. We detected slightly more clusters with (0.5-2.0keV) X-ray fluxes of >2x10–14erg/s/cm2 than we expected based on expectations from deep ROSAT surveys. We also present the luminosity-temperature relation for our nine brightest objects possessing a reliable temperature determination. The slope is in good agreement with the local relation, yet compatible with a luminosity enhancement for the 0.15 < z < 0.35 objects having 1 < T < 2keV, a population that the XMM-LSS is identifying systematically for the first time. The present study permits the compilation of cluster samples from XMM images whose selection biases are understood. This allows, in addition to studies of large-scale structure, the systematic investigation of cluster scaling law evolution, especially for low mass X-ray groups which constitute the bulk of our observed cluster population. All cluster ancillary data (images, profiles, spectra) are made available in electronic form via the XMM-LSS cluster data base.
2006 The Authors. Journal compilation © 2006 RAS
surveys - X-rays: galaxies: clusters
Tables 3, 4: [PPD2006] Cluster a (Nos a-d).
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