Combined analysis of weak lensing and X-ray blind surveys
Combined analysis of weak lensing and X-ray blind surveys
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DOI：
10.1111/j.1365-2966.2008.12902.x
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发表时间：
2007-12
影响因子：
4.8
通讯作者：
J. Berg'e;F. Pacaud;Alexandre R'efr'egier;R. Massey;M. Pierre;A. Amara;M. Birkinshaw;S. Paulin-Henriksson;Graham P. Smith;J. P. I. F. Astronomy;Bonn Caltech University of Bristol University of Birmin Victoria-Bonn-Caltech-University-of-Bristol-University-of-121343140
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文献类型：
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作者：
J. Berg'e;F. Pacaud;Alexandre R'efr'egier;R. Massey;M. Pierre;A. Amara;M. Birkinshaw;S. Paulin-Henriksson;Graham P. Smith;J. P. I. F. Astronomy;Bonn Caltech University of Bristol University of Birmin Victoria-Bonn-Caltech-University-of-Bristol-University-of-121343140
我们提供了一个来自CFHTLS和XMMLSS巡天的4度^2的弱透镜和X射线联合分析。我们的弱透镜分析是第一次分析的真实的调查使用shapeling，新一代弱透镜分析方法。我们创建了图像的投影质量图，并提取了六个弱透镜检测到的星系团。我们证明了它们的计数可以用来限制功率谱归一化σ8 = 0.92^（+0.26）_（-0.30）（其中λ m = 0.24）。我们表明，尽管大的散射一般观察到的质量-温度（MT）的关系来自透镜质量，严格的约束，其斜率和归一化M可以得到一个中等数量的源，只要覆盖的质量范围足够大。将Bardeau等人给出的簇添加到我们的样本中，我们测得M =2.71^（+0.79）_（-0.61）× 10^（14）h^（-1）M。虽然它们主要是由散粒噪声和样本方差，我们的测量是一致的，目前青睐的值，并为未来的调查奠定了基础。因此，我们调查的依赖性，这些估计的调查规模，深度和整合时间，联合弱透镜和X射线调查。我们表明，深调查应致力于研究星系团和星系群的物理。对于一个给定的曝光时间，广泛的调查提供了大量的检测到的集群，因此是首选的宇宙学参数的测量，如σ8和M。我们表明，需要一个几百平方度的广泛的调查，以改善目前的测量这些参数。覆盖7000度^[2]的更大范围的测量将在功率谱估计和M-T关系归一化方面提供1%的精度。
We present a joint weak lensing and X-ray analysis of 4 deg^2 from the CFHTLS and XMMLSS 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)_(−0.61) × 10^(14) h^(−1) Mסּ. 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 deg^2 will provide the 1 per cent accuracy in the estimation of the power-spectrum and the M–T relation normalizations.