Testing for X-Ray–SZ Differences and Redshift Evolution in the X-Ray Morphology of Galaxy Clusters
Testing for X-Ray–SZ Differences and Redshift Evolution in the X-Ray Morphology of Galaxy Clusters
复制标题
测试星系团 X 射线形态中的 X 射线 SZ 差异和红移演化
DOI：
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
A. Vikhlinin
中科院分区：
文献类型：
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作者：
D. Nurgaliev;M. Mcdonald;B. Benson;L. Bleem;S. Bocquet;W. Forman;G. Garmire;N. Gupta;J. Hlavacek;J. Mohr;D. Nagai;D. Rapetti;A. Stark;C. Stubbs;A. Vikhlinin
我们提出了星系团的x射线形态的定量研究，作为它们的检测方法和红移的函数。我们分析了两个独立的星系团样本：一个是通过ROSAT PSPC 400°2调查在x射线中选择的36个星系团样本，另一个是通过南极望远镜通过Sunyaev-Zel 'dovich （SZ）效应选择的90个星系团样本。来自两个样本的簇具有相似质量的钱德拉观测，这使我们能够通过两种不同的方法量化它们的x射线形态：质心位移(w)和光子不对称（）。后一种技术为跨越广泛红移和数据质量的簇提供了几乎无偏的形态学估计。我们进一步比较了x射线和sz选择的簇与模拟簇的x射线形态。在这些样品探测的红移范围内，我们没有发现x射线和sz选择的星团的测量x射线形态在统计上有显著差异，这表明两者正在探测相似的星团群。我们发现模拟星团的x射线形态在统计上与x射线或sz选择的星团无法区分，这意味着在这些模拟中很好地近似了决定大规模气体形态（核心外）的最重要物理。最后，我们发现在x射线形态（无论是观测到的还是模拟的星团）中没有统计学上显著的红移演化，在到的范围内，这似乎与模拟预测的红移依赖光晕合并率相矛盾。
We present a quantitative study of the X-ray morphology of galaxy clusters, as a function of their detection method and redshift. We analyze two separate samples of galaxy clusters: a sample of 36 clusters at selected in the X-ray with the ROSAT PSPC 400 deg2 survey, and a sample of 90 clusters at selected via the Sunyaev–Zel’dovich (SZ) effect with the South Pole Telescope. Clusters from both samples have similar-quality Chandra observations, which allow us to quantify their X-ray morphologies via two distinct methods: centroid shifts (w) and photon asymmetry ( ). The latter technique provides nearly unbiased morphology estimates for clusters spanning a broad range of redshift and data quality. We further compare the X-ray morphologies of X-ray- and SZ-selected clusters with those of simulated clusters. We do not find a statistically significant difference in the measured X-ray morphology of X-ray and SZ-selected clusters over the redshift range probed by these samples, suggesting that the two are probing similar populations of clusters. We find that the X-ray morphologies of simulated clusters are statistically indistinguishable from those of X-ray- or SZ-selected clusters, implying that the most important physics for dictating the large-scale gas morphology (outside of the core) is well-approximated in these simulations. Finally, we find no statistically significant redshift evolution in the X-ray morphology (both for observed and simulated clusters), over the range of to , seemingly in contradiction with the redshift-dependent halo merger rate predicted by simulations.
影响因子：
6.5
作者：
Joana S. Santos;P. Tozzi;P. Rosati;H. Boehringer
通讯作者：
Joana S. Santos;P. Tozzi;P. Rosati;H. Boehringer
影响因子：
8.7
作者：
Komatsu, E.;Smith, K. M.;Wright, E. L.
通讯作者：
Wright, E. L.
星系团中的 LXâTvir 关系：辐射冷却和 AGN 加热的影响
影响因子：
6.5
作者：
Mittal;Reiprich;Jaritz
通讯作者：
Jaritz