Mon. Not. R. Astron. Soc., 385, 695-707 (2008/April-1)
Combined analysis of weak lensing and X-ray blind surveys.
BERGE J., PACAUD F., REFREGIER A., MASSEY R., PIERRE M., AMARA A., BIRKINSHAW M., PAULIN-HENRIKSSON S., SMITH G.P. and WILLIS J.
Abstract (from CDS):
We present a joint weak lensing and X-ray analysis of 4 deg2 from the CFHTLS and XMM-LSS surveys. Our weak lensing analysis is the first analysis of a real survey using shapelets, a new generation weak lensing analysis method. We create projected mass maps of the images, and extract six weak-lensing-detected clusters of galaxies. We show that their counts can be used to constrain the power-spectrum normalization σ8= 0.92+0.26–0.30 for Ωm= 0.24. We show that despite the large scatter generally observed in the mass-temperature (M-T) relation derived from lensing masses, tight constraints on both its slope and normalization M* can be obtained with a moderate number of sources provided that the covered mass range is large enough. Adding clusters given by Bardeau et al. to our sample, we measure M*= 2.71+0.79–0.61x1014h–1Msolar. Although they are dominated by shot noise and sample variance, our measurements are consistent with currently favoured values, and set the stage for future surveys. We thus investigate the dependence of those estimates on survey size, depth and integration time, for joint weak lensing and X-ray surveys. We show that deep surveys should be dedicated to the study of the physics of clusters and groups of galaxies. For a given exposure time, wide surveys provide a larger number of detected clusters and are therefore preferred for the measurement of cosmological parameters, such as σ8 and M*. We show that a wide survey of a few hundred square degrees is needed to improve upon current measurements of these parameters. More ambitious surveys covering 7000 deg2 will provide the 1 per cent accuracy in the estimation of the power-spectrum and the M-T relation normalizations.
2008 The Authors. Journal compilation © 2008 RAS
gravitational lensing - surveys - cosmological parameters - dark matter - large-scale structure of Universe - X-rays: galaxies: clusters
Table 1: [BPR2008] WLNN (Nos WL01-WL07).
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