The redshift evolution of massive galaxy clusters in the MACSIS simulations
The redshift evolution of massive galaxy clusters in the MACSIS simulations
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MACSIS 模拟中大质量星系团的红移演化
DOI：
10.1093/mnras/stw2722
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发表时间：
2017
影响因子：
4.8
通讯作者：
Barnes D
中科院分区：
文献类型：
--
作者：
Barnes D
我们提出了大规模的星系团和星系团间结构（MACSIS）项目，一套390个集群模拟重子物理，产生现实的大规模星系团能够匹配广泛的观察到的属性。MACSIS将最近的BAHAMAS模拟扩展到更高的质量，从而能够对星系团性质的红移演化进行稳健的预测，并评估仅选择最热系统的影响。在完整的观测质量范围内，我们研究了观测质量标度关系和X射线光温关系。正如预期的那样，我们发现这些标度关系的斜率和它们的归一化与红移的演变显着偏离自相似的预测。然而，对于具有核心切除温度的热星团样本，可观测质量关系的归一化和斜率及其演化显着更接近自相似。例外的是温度-质量关系，其中非热压力支持和偏置X射线温度的重要性增加导致在最热的系统中更大地偏离自相似性。因此，这些也影响亮度-温度关系中归一化的斜率和演变。中值热气剖面在= 0和= 1时与观测数据吻合良好，其演化再次显著偏离自相似预测。然而，选择一个热样本的集群产生的配置文件，演变显着更接近自相似的预测。总之，我们的研究结果表明，理解选择函数是至关重要的强大的质量和红移的集群属性的校准。
We present the MAssive ClusterS and Intercluster Structures (MACSIS) project, a suite of 390 clusters simulated with baryonic physics that yields realistic massive galaxy clusters capable of matching a wide range of observed properties. MACSIS extends the recent BAHAMAS simulation to higher masses, enabling robust predictions for the redshift evolution of cluster properties and an assessment of the effect of selecting only the hottest systems. We study the observable-mass scaling relations and the X-ray luminosity-temperature relation over the complete observed cluster mass range. As expected, we find the slope of these scaling relations and the evolution of their normalization with redshift departs significantly from the self-similar predictions. However, for a sample of hot clusters with core-excised temperaturesthe normalization and slope of the observable-mass relations and their evolution are significantly closer to self-similar. The exception is the temperature-mass relation, for which the increased importance of non-thermal pressure support and biased X-ray temperatures leads to a greater departure from self-similarity in the hottest systems. As a consequence, these also affect the slope and evolution of the normalization in the luminosity-temperature relation. The median hot gas profiles show good agreement with observational data at= 0 and= 1, with their evolution again departing significantly from the self-similar prediction. However, selecting a hot sample of clusters yields profiles that evolve significantly closer to the self-similar prediction. In conclusion, our results show that understanding the selection function is vital for robust calibration of cluster properties with mass and redshift.
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DOI：
10.1111/j.1365-2966.2010.17573.x
发表时间：
2010-01
影响因子：
4.8
作者：
J. Courtin;Y. Rasera;J. Alimi;Pier Stefano Corasaniti;V. Boucher;A. Fűzfa
通讯作者：
J. Courtin;Y. Rasera;J. Alimi;Pier Stefano Corasaniti;V. Boucher;A. Fűzfa
星系团 II 的音乐：X 射线全局属性和标度关系
DOI：
--
发表时间：
2014
期刊：
影响因子：
--
作者：
V. Biffi;F. Sembolini;M. Petris;R. Valdarnini;G. Yepes;S. Gottlober
通讯作者：
S. Gottlober
星系团X射线标度关系的演化
DOI：
10.1111/j.1365-2966.2010.17267.x
发表时间：
2010
影响因子：
4.8
作者：
C. Short;P. Thomas;O. Young;F. Pearce;A. Jenkins;O. M. U. O. Sussex;UK.;U. Nottingham;U. Durham;Khon Kaen University;Thailand
通讯作者：
Thailand
根据 X 射线和 Sunyaev-Zeldovich 观测测量的压力剖面中气体不均匀性造成的偏差
影响因子：
4.8
作者：
S. Khedekar;E. Churazov;A. Kravtsov;I. Zhuravleva;E. Lau;D. Nagai;R. Sunyaev
通讯作者：
R. Sunyaev
模拟星系团种群全球热气特性的散射与演化
影响因子：
4.8
作者：
A. Brun;I. McCarthy;J. Schaye;T. Ponman
通讯作者：
T. Ponman