WEAK LENSING MEASUREMENT OF GALAXY CLUSTERS IN THE CFHTLS-WIDE SURVEY
WEAK LENSING MEASUREMENT OF GALAXY CLUSTERS IN THE CFHTLS-WIDE SURVEY
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DOI：
10.1088/0004-637x/748/1/56
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发表时间：
2011-08
期刊：
影响因子：
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通讯作者：
H. Shan;J. Kneib;C. Tao;Z. Fan;M. Jauzac;M. Limousin;R. Massey;J. Rhodes;K. Thanjavur;
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文献类型：
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作者：
H. Shan;J. Kneib;C. Tao;Z. Fan;M. Jauzac;M. Limousin;R. Massey;J. Rhodes;K. Thanjavur;
我们给出了完成的加拿大-法国-夏威夷望远镜遗产调查(CFHTLS)的第一个弱引力透镜分析。我们研究了CFHTLS最大的观测场--W1场，并给出了迄今制作的最大的连续弱透镜会聚“质量图”。使用凯撒-斯奎尔斯和布罗德赫斯特方法(KSB)管道测量了266万个星系形状，并与覆盖部分CFHTLS的高分辨率哈勃太空望远镜成像进行了验证。我们的I‘波段测量也与独立R’波段成像的分析一致。重建的透镜会聚图包含301个峰值，信噪比为ν>；3.5，与Λ清洁发展机制模型的预测一致。在这些峰中，有126个位于一个最明亮的中央星系的3.‘0范围内，这是一项独立的红色序列调查中通过多色光学成像确定的。我们还确定了之前在6°2 XMM-LSS调查范围内的X射线发射中看到的大质量星系团的七个对应物。根据源星系的光度学红移估计，我们使用层析透镜方法来拟合每个会聚峰的红移和质量。与光学观测相匹配，我们确认了85个群/星系团，其平均红移<zc>=0.36，速度色散<χc>=658.8 kM Sσ1。未来的调查，如DES，LSST，KDUST和欧几里德，将能够应用这些技术来绘制更大体积的星系团图，从而严格约束宇宙学模型。
We present the first weak gravitational lensing analysis of the completed Canada–France–Hawaii Telescope Legacy Survey (CFHTLS). We study the 64 deg2 W1 field, the largest of the CFHTLS-Wide survey fields, and present the largest contiguous weak lensing convergence “mass map” yet made. 2.66 million galaxy shapes are measured, using the Kaiser Squires and Broadhurst Method (KSB) pipeline verified against high-resolution Hubble Space Telescope imaging that covers part of the CFHTLS. Our i′-band measurements are also consistent with an analysis of independent r′-band imaging. The reconstructed lensing convergence map contains 301 peaks with signal-to-noise ratio ν > 3.5, consistent with predictions of a ΛCDM model. Of these peaks, 126 lie within 3.′0 of a brightest central galaxy identified from multicolor optical imaging in an independent, red sequence survey. We also identify seven counterparts for massive clusters previously seen in X-ray emission within 6 deg2 XMM-LSS survey. With photometric redshift estimates for the source galaxies, we use a tomographic lensing method to fit the redshift and mass of each convergence peak. Matching these to the optical observations, we confirm 85 groups/clusters with χ2reduced < 3.0, at a mean redshift 〈zc〉 = 0.36 and velocity dispersion 〈σc〉 = 658.8 km s−1. Future surveys, such as DES, LSST, KDUST, and EUCLID, will be able to apply these techniques to map clusters in much larger volumes and thus tightly constrain cosmological models.