The XXL Survey
The XXL Survey
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XXL 调查
DOI：
10.1051/0004-6361/201526891
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
Reiprich
中科院分区：
文献类型：
--
作者：
Pacaud;. . . ;Reiprich
XXL测量是xmm -牛顿卫星进行的最大的测量，覆盖总面积为50平方度，分布在两个领域。它主要目的是利用星系团和活动星系核的分布作为物质分布的示踪剂来研究宇宙的大尺度结构。该调查最终将在[0.5-2]keV波段以~ 10−14 erg s−1cm−2的灵敏度发现数百个红移为~ 2的星系团。本文给出了从整个XXL星表中选取的100个星系团的子样本——XXL明亮星系团样本，该样本在1孔径内的源通量下限为3× 10−14 erg s−1 cm−2。方法采用蒙特卡罗模拟和近似再现源选择过程的分析方法相结合的方法估计选择函数。对100个星团中的97个进行了广泛的光谱追踪，发现了红移现象。我们得到了所有光源的精确x射线参数。比例关系自一致地从该系列的其他出版物的相同样本中得出。在此基础上，研究了样品的数量密度、光度函数和空间分布。结果明亮星团样本由质量在M500= 7× 1013 ~ 3× 1014 M⊙之间的系统组成，大部分位于z= 0.1 ~ 0.5之间。观测到的星团的天空密度略低于WMAP9模型的预测，明显低于普朗克2015宇宙学的预测。一般来说，在当前的聚类质量校准不确定度范围内，σ8和/或ΩM值越高的模型越难以适应。我们对星团微分光度函数提供了严格的约束，并没有发现z ~ 1以内的演化迹象。我们还发现了在XXL明亮星团样本中存在大规模结构的有力证据，并确定了五个新的超星团。
ContextThe XXL Survey is the largest survey carried out by the XMM-Newton satellite and covers a total area of 50 square degrees distributed over two fields. It primarily aims at investigating the large-scale structures of the Universe using the distribution of galaxy clusters and active galactic nuclei as tracers of the matter distribution. The survey will ultimately uncover several hundreds of galaxy clusters out to a redshift of∼ 2 at a sensitivity of∼ 10− 14 erg s− 1cm− 2 in the [0.5-2] keV band.AimsThis article presents the XXL bright cluster sample, a subsample of 100 galaxy clusters selected from the full XXL catalogue by setting a lower limit of 3× 10− 14 erg s− 1 cm− 2 on the source flux within a 1 aperture.MethodsThe selection function was estimated using a mixture of Monte Carlo simulations and analytical recipes that closely reproduce the source selection process. An extensive spectroscopic follow-up provided redshifts for 97 of the 100 clusters. We derived accurate X-ray parameters for all the sources. Scaling relations were self-consistently derived from the same sample in other publications of the series. On this basis, we study the number density, luminosity function, and spatial distribution of the sample.ResultsThe bright cluster sample consists of systems with masses between M500= 7× 1013 and 3× 1014 M⊙, mostly located between z= 0.1 and 0.5. The observed sky density of clusters is slightly below the predictions from the WMAP9 model, and significantly below the prediction from the Planck 2015 cosmology. In general, within the current uncertainties of the cluster mass calibration, models with higher values of σ8 and/or ΩM appear more difficult to accommodate. We provide tight constraints on the cluster differential luminosity function and find no hint of evolution out to z∼ 1. We also find strong evidence for the presence of large-scale structures in the XXL bright cluster sample and identify five new superclusters.
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影响因子：
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作者：
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DOI：
--
发表时间：
2015
期刊：
影响因子：
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作者：
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DOI：
--
发表时间：
1966
期刊：
影响因子：
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作者：
K. Kellermann
通讯作者：
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DOI：
--
发表时间：
2005
期刊：
影响因子：
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作者：
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