The XMM-LSS survey: optical assessment and properties of different X-ray selected cluster classes
The XMM-LSS survey: optical assessment and properties of different X-ray selected cluster classes
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DOI：
10.1051/0004-6361/201015182
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发表时间：
2010-10
影响因子：
6.5
通讯作者：
C. Adami;A. Mazure;M. Pierre;P. Sprimont;C. Libbrecht;F. Pacaud;F. Pacaud;N. Clerc;T. Sadibekova;J. Surdej;B. Altieri;P. Duc;G. Galaz;A. Gueguen;L. Guennou;G. Hertling;O. Ilbert;J. Fèvre;H. Quintana;I. Valtchanov;J. Willis;Masayuki Akiyama;H. Aussel;L. Chiappetti;A. Detal;B. Garilli;V. Lebrun;O. LeFèvre;D. Maccagni;J. Melin;T. Ponman;D. Ricci;L. Tresse
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文献类型：
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作者：
C. Adami;A. Mazure;M. Pierre;P. Sprimont;C. Libbrecht;F. Pacaud;F. Pacaud;N. Clerc;T. Sadibekova;J. Surdej;B. Altieri;P. Duc;G. Galaz;A. Gueguen;L. Guennou;G. Hertling;O. Ilbert;J. Fèvre;H. Quintana;I. Valtchanov;J. Willis;Masayuki Akiyama;H. Aussel;L. Chiappetti;A. Detal;B. Garilli;V. Lebrun;O. LeFèvre;D. Maccagni;J. Melin;T. Ponman;D. Ricci;L. Tresse
语境。 XMM 和钱德拉为星系团研究开辟了一个新领域，不仅用于星系团物理，还用于探测以前的任务无法到达的微弱和遥远的星系团。目标。本文介绍了 XMM-LSS 勘测所包含的 6 deg(2) 区域内的 66 个经光谱确认的星团 (0.05 \textless= z \textless= 1.5)。近三分之二仅通过专用光谱得到证实，10% 已通过专用光谱辅以文献红移得到证实。方法。扩展源的子样本或类别在二维 X 射线参数空间中定义，允许不同程度的完整性和污染。我们描述了使用 CFHTLS 光度数据和我们自己的后续活动的光谱信息来评估这些候选星团的真实性的程序。结果。大多数这些天体都是低质量星团，因此构成了一个尚未得到充分研究的群体。第二步，我们量化光学特性（例如丰富度或速度色散）与星团 X 射线光度之间的相关性。我们研究星团与宇宙网的关系。最后，我们回顾了调查区域中特有的致密结构，例如非常遥远的星团和化石群。
Context. XMM and Chandra opened a new area for the study of clusters of galaxies not only for cluster physics, but also for the detection of faint and distant clusters that were inaccessible with previous missions. Aims. This article presents 66 spectroscopically confirmed clusters (0.05 \textless= z \textless= 1.5) within an area of 6 deg(2) enclosed in the XMM-LSS survey. Almost two thirds have been confirmed with dedicated spectroscopy only and 10% have been confirmed with dedicated spectroscopy supplemented by literature redshifts. Methods. Sub-samples, or classes, of extended-sources are defined in a two-dimensional X-ray parameter space allowing for various degrees of completeness and contamination. We describe the procedure developed to assess the reality of these cluster candidates using the CFHTLS photometric data and spectroscopic information from our own follow-up campaigns. Results. Most of these objects are low-mass clusters, hence constituting a still poorly studied population. In a second step, we quantify the correlations between the optical properties such as richness or velocity dispersion and the cluster X-ray luminosities. We examine the relation of the clusters to the cosmic web. Finally, we review peculiar compact structures in the surveyed area such as very distant clusters and fossil groups.