THE REDSHIFT EVOLUTION OF THE MEAN TEMPERATURE, PRESSURE, AND ENTROPY PROFILES IN 80 SPT-SELECTED GALAXY CLUSTERS
THE REDSHIFT EVOLUTION OF THE MEAN TEMPERATURE, PRESSURE, AND ENTROPY PROFILES IN 80 SPT-SELECTED GALAXY CLUSTERS
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80 个 SPT 选定的星系团中平均温度、压力和熵剖面的红移演化
DOI：
10.1088/0004-637x/794/1/67
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
A. Zenteno
中科院分区：
文献类型：
--
作者：
M. McDonald;B. Benson;A. Vikhlinin;K. Aird;S. Allen;M. Bautz;M. Bayliss;L. Bleem;S. Bocquet;M. Brodwin;J. Carlstrom;C. Chang;H. Cho;A. Clocchiatti;T. Crawford;A. Crites;T. de Haan;M. Dobbs;R. Foley;W. Forman;E. George;M. Gladders;A. Gonzalez;N. Halverson;J. Hlavacek;G. Holder;W. Holzapfel;J. Hrubeš;C. Jones;R. Keisler;L. Knox;A. Lee;E. Leitch;J. Liu;M. Lueker;D. Luong;A. Mantz;D. Marrone;J. McMahon;S. Meyer;E. Miller;L. Mocanu;J. Mohr;S. Murray;S. Padin;C. Pryke;C. Reichardt;A. Rest;J. Ruhl;B. Saliwanchik;A. Saro;J. Sayre;K. Schaffer;E. Shirokoff;H. Spieler;B. Stalder;S. Stanford;Z. Staniszewski;A. Stark;K. Story;C. Stubbs;K. Vanderlinde;J. Vieira;R. Williamson;O. Zahn;A. Zenteno
我们提出了一个X射线分析的结果，80个星系团选择在2500 deg 2南极望远镜调查和观察钱德拉X射线天文台。我们将完整的样本分为子样本的基础上红移和中心密度的200个集群，同时进行联合X射线光谱拟合子样本中的所有集群，假设自相似的温度分布。这种方法允许我们将温度分布的形状限制在0 < r < 1.5R500，这在每个集群的基础上是不可能的，因为单个集群的观测平均有2000个X射线计数。这里给出的结果代表的平均温度分布从z = 0到z = 1.2的演变的第一个约束。我们发现高z（0.6 < z < 1.2）团簇在内部（r < 0.1R500）和外部（r > R500）区域都比低z（0.3 < z < 0.6）团簇稍微冷（约30%）。结合平均温度分布与测量的气体密度分布从我们早期的工作，我们推断出的平均压力和熵分布为每个子样本。从这个数据集的早期结果，我们发现在高z没有强冷核心，表现在这个分析作为一个显着较低的观察到的压力在中央0.1R500的高z冷核心集群子集相比，低z冷核心子集。总的来说，我们观察到的压力分布与早期的低红移测量结果吻合得很好，这表明核心外的压力分布中的红移演化最小。我们发现在r = 0.7R500的熵分布中没有可测量的红移演化-这可能反映了在长时间尺度和大物理尺度上冷却和反馈之间的长期平衡。在我们的高z子样本中，我们观察到在r = R500处熵分布略微平坦。这种扁平化与温度偏差是一致的，因为群质量（1.2 keV）晕（在我们的调查深度处无法检测到）在z 1处吸积到星系团上的速率增强（1.3 ×）。这项工作展示了一个强大的方法推断空间分辨集群属性的情况下，个别集群的信噪比低，但观察到的集群的数量是高的。
We present the results of an X-ray analysis of 80 galaxy clusters selected in the 2500 deg2 South Pole Telescope survey and observed with the Chandra X-ray Observatory. We divide the full sample into subsamples of ∼20 clusters based on redshift and central density, performing a joint X-ray spectral fit to all clusters in a subsample simultaneously, assuming self-similarity of the temperature profile. This approach allows us to constrain the shape of the temperature profile over 0 < r < 1.5R500, which would be impossible on a per-cluster basis, since the observations of individual clusters have, on average, 2000 X-ray counts. The results presented here represent the first constraints on the evolution of the average temperature profile from z = 0 to z = 1.2. We find that high-z (0.6 < z < 1.2) clusters are slightly (∼30%) cooler both in the inner (r < 0.1R500) and outer (r > R500) regions than their low-z (0.3 < z < 0.6) counterparts. Combining the average temperature profile with measured gas density profiles from our earlier work, we infer the average pressure and entropy profiles for each subsample. Confirming earlier results from this data set, we find an absence of strong cool cores at high z, manifested in this analysis as a significantly lower observed pressure in the central 0.1R500 of the high-z cool-core subset of clusters compared to the low-z cool-core subset. Overall, our observed pressure profiles agree well with earlier lower-redshift measurements, suggesting minimal redshift evolution in the pressure profile outside of the core. We find no measurable redshift evolution in the entropy profile at r ≲ 0.7R500—this may reflect a long-standing balance between cooling and feedback over long timescales and large physical scales. We observe a slight flattening of the entropy profile at r ≳ R500 in our high-z subsample. This flattening is consistent with a temperature bias due to the enhanced (∼3×) rate at which group-mass (∼2 keV) halos, which would go undetected at our survey depth, are accreting onto the cluster at z ∼ 1. This work demonstrates a powerful method for inferring spatially resolved cluster properties in the case where individual cluster signal-to-noise is low, but the number of observed clusters is high.
DOI：
10.1088/0004-637x/722/2/1180
发表时间：
2010-03
期刊：
The Astrophysical Journal
影响因子：
--
作者：
F. W. High;B. Stalder;J. Song;P. Ade;K. Aird;S. Allam;R. Armstrong;W. Barkhouse;B. Benson;B. Benson;E. Bertin;Suman Bhattacharya;L. Bleem;M. Brodwin;E. Buckley-Geer;J. Carlstrom;P. Challis;C. Chang;T. Crawford;A. Crites;T. Haan;S. Desai;M. Dobbs;J. Dudley;R. Foley;E. George;M. Gladders;N. Halverson;M. Hamuy;S. Hansen;G. Holder;W. Holzapfel;J. Hrubeš;M. Joy;R. Keisler;Adrian T. Lee;Adrian T. Lee;E. Leitch;Huan Lin;Yen-Ting Lin;A. Loehr;M. Lueker;D. Marrone;J. McMahon;J. McMahon;J. Mehl;S. Meyer;J. J. Mohr-J.;T. Montroy;N. Morell;C. Ngeow;S. Padin;T. Plagge;T. Plagge;C. Pryke;C. Reichardt;A. Rest;J. Ruel;J. Ruhl;K. Schaffer;L. Shaw;L. Shaw;E. Shirokoff;R. C. Smith;H. Spieler;Z. Staniszewski;A. Stark;C. Stubbs;D. Tucker;K. Vanderlinde;J. Vieira;R. Williamson;W. M. Wood-Vasey;Y. Yang;O. Zahn;A. Zenteno
通讯作者：
F. W. High;B. Stalder;J. Song;P. Ade;K. Aird;S. Allam;R. Armstrong;W. Barkhouse;B. Benson;B. Benson;E. Bertin;Suman Bhattacharya;L. Bleem;M. Brodwin;E. Buckley-Geer;J. Carlstrom;P. Challis;C. Chang;T. Crawford;A. Crites;T. Haan;S. Desai;M. Dobbs;J. Dudley;R. Foley;E. George;M. Gladders;N. Halverson;M. Hamuy;S. Hansen;G. Holder;W. Holzapfel;J. Hrubeš;M. Joy;R. Keisler;Adrian T. Lee;Adrian T. Lee;E. Leitch;Huan Lin;Yen-Ting Lin;A. Loehr;M. Lueker;D. Marrone;J. McMahon;J. McMahon;J. Mehl;S. Meyer;J. J. Mohr-J.;T. Montroy;N. Morell;C. Ngeow;S. Padin;T. Plagge;T. Plagge;C. Pryke;C. Reichardt;A. Rest;J. Ruel;J. Ruhl;K. Schaffer;L. Shaw;L. Shaw;E. Shirokoff;R. C. Smith;H. Spieler;Z. Staniszewski;A. Stark;C. Stubbs;D. Tucker;K. Vanderlinde;J. Vieira;R. Williamson;W. M. Wood-Vasey;Y. Yang;O. Zahn;A. Zenteno
通过广域 XMM 星团巡天进行精密宇宙学
DOI：
10.1111/j.1365-2966.2011.18511.x
发表时间：
2011
影响因子：
4.8
作者：
Pierre
通讯作者：
Pierre