Probing the dark-matter halos of cluster galaxies with weak lensing
Probing the dark-matter halos of cluster galaxies with weak lensing
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DOI：
10.1051/0004-6361/201116851
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发表时间：
2011-03
影响因子：
6.5
通讯作者：
E. P. Mira;S. Hilbert;J. Hartlap;P. Schneider
中科院分区：
文献类型：
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作者：
E. P. Mira;S. Hilbert;J. Hartlap;P. Schneider
上下文了解星系成为星系团一部分后暗物质晕的演化对于了解这些卫星星系的演化至关重要。目标。我们研究了星系-星系透镜效应在绘制星系团中星系晕密度分布图方面的潜力。方法.我们提出了一种方法，分离星系团中的暗物质晕的弱透镜信号的星系团的主晕的弱透镜信号。使用玩具集群模型以及射线跟踪通过N体模拟结构形成沿着与半解析星系形成模型，我们测试的方法，并评估其性能。结果我们表明，与所提出的方法，可以恢复的星系团星系晕的密度分布在30 - 300千秒差距的范围。利用该方法，我们发现在千禧年模拟中，星系团成员星系的弱透镜信号可以用Navarro-Frenk-白色（NFW）轮廓很好地描述。相比之下，非奇异等温质量分布（如PIEMD）模型提供了较差的拟合。此外，我们没有发现证据的急剧截断的星系晕的范围内探测我们的方法。相反，有一个观察到的整体减少的星系团成员星系的晕质量分布随着时间的增加，在集群中度过。这种趋势，以及截断半径的存在或不存在，应该可以在未来的弱透镜调查中检测到，如暗能量调查（DES）或大型综合巡天望远镜（LSST）调查。这样的调查也应该允许一个推断的质量-光度关系的星系团星系与我们的方法超过20年的质量。结论.利用我们提出的弱透镜方法，有可能在未来的巡天中以非参数方式恢复卫星星系及其暗物质晕的质量分布。
Context. Understanding the evolution of the dark matter halos of galaxies after they become part of a cluster is essential for understanding the evolution of these satellite galaxies. Aims. We investigate the potential of galaxy-galaxy lensing to map the halo density profiles of galaxies in clusters. Methods. We propose a method that separates the weak-lensing signal of the dark-matter halos of galaxies in clusters from the weaklensing signal of the cluster’s main halo. Using toy cluster models as well as ray-tracing through N-body simulations of structure formation along with semi-analytic galaxy formation models, we test the method and assess its performance. Results. We show that with the proposed method, one can recover the density profiles of the cluster galaxy halos in the range 30– 300 kpc. Using the method, we find that the weak-lensing signal of cluster member galaxies in the Millennium Simulation is well described by a Navarro-Frenk-White (NFW) profile. In contrast, non-singular isothermal mass distribution (like PIEMD) models provide a poor fit. Furthermore, we do not find evidence for a sharp truncation of the galaxy halos in the range probed by our method. Instead, there is an observed overall decrease of the halo mass profile of cluster member galaxies with increasing time spent in the cluster. This trend, as well as the presence or absence of a truncation radius, should be detectable in future weak-lensing surveys like the Dark Energy Survey (DES) or the Large Synoptic Survey Telescope (LSST) survey. Such surveys should also allow one to infer the mass-luminosity relation of cluster galaxies with our method over two decades in mass. Conclusions. It is possible to recover in a non-parametric way the mass profile of satellite galaxies and their dark matter halos in future surveys, using our proposed weak lensing method.