Exploring the Bridge between A3556 and A3558 in the Shapley Supercluster
Exploring the Bridge between A3556 and A3558 in the Shapley Supercluster
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探索沙普利超星系团中 A3556 和 A3558 之间的桥梁
DOI：
10.1088/0004-637x/806/2/211
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发表时间：
2015
期刊：
影响因子：
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通讯作者：
K. Sato
中科院分区：
文献类型：
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作者：
E. Ursino;M. Galeazzi;A. Gupta;R. L. Kelley;I. Mitsuishi;T. Ohashi;K. Sato
观察连接两个星系团的区域是识别和研究温热星系际介质的一种有前途的方法。观测结果表明，A3556和A3558之间的桥的光谱具有比附近区域更强的软X射线发射。朱雀的观测无法区分额外发射的来源。在这项工作中，我们分析了一个专门的钱德拉观察同一目标，以确定点源和特征的背景发射的桥梁。我们发现，点源的计数数远高于平均场布居数（以CDFS 4 M为参考）。此外，累积分布的形状类似于星系分布，这表明点源是在一个灯丝星系。朱雀星的额外辐射可以很好地解释为钱德拉发现的高丰度点源。此外，我们使用同一场中的点源的光学/红外观测来估计假定的暗条的密度，
Looking at the region connecting two clusters is a promising way to identify and study the Warm–Hot Intergalactic Medium. Observations show that the spectrum of the bridge between A3556 and A3558 has a stronger soft X-ray emission than the nearby region. Suzaku observations could not discriminate the origin of the extra emission. In this work we analyze a dedicated Chandra observation of the same target to identify point sources and characterize the background emission in the bridge. We find that the count number of the point sources is much higher than average field population (using CDFS 4 Ms as a reference). Moreover, the shape of the cumulative distribution resembles that of galaxy distribution suggesting that the point sources are galaxies in a filament. The Suzaku extra emission is well explained by the high abundance of point sources identified by Chandra. Furthermore, we used optical/IR observations of point sources in the same field to estimate the density of the putative filament as