XMM-Newton Observation of IC 310 in the Outer Region of the Perseus Cluster of Galaxies
XMM-Newton Observation of IC 310 in the Outer Region of the Perseus Cluster of Galaxies
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DOI：
10.1093/pasj/57.5.743
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发表时间：
2005-09
影响因子：
2.3
通讯作者：
K. Sato;T. Furusho;N. Yamasaki;M. Ishida;K. Matsushita;T. Ohashi
中科院分区：
文献类型：
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作者：
K. Sato;T. Furusho;N. Yamasaki;M. Ishida;K. Matsushita;T. Ohashi
我们给出了对位于英仙座星系团西南部的头部-尾部射电星系IC310的XMM-牛顿观测结果。光谱符合吸收幂定律模型，其光子指数为2.50±0.02，没有明显的吸收过剩。X射线图像显示了IC310的点状发射，没有任何迹象表明与射电晕尾相关的结构。IC310周围星团内介质的温度随距离星团中心的距离而下降，从视场东北角的KT∼6keV下降到西南区的约3keV。虽然我们在表面亮度分布中没有发现任何锐利的边缘，但可以看到比平滑β模型高出约20%的亮度。同一地区的气温也上升了10%左右。这表明IC310区域是一个可能流入英仙座星系团的子星系团，IC310前面朝向英仙座星系团的气体很可能被大尺度运动压缩，这支持了IC310系统正在经历合并的观点。
We present results from an XMM-Newton observation of the head-tail radio galaxy IC 310 located in the southwest region of the Perseus cluster. The spectrum is well fitted by an absorbed power-law model with a photon index of 2.50 ±0.02 without significant absorption excess. The X-ray image shows a point-like emission at IC 310 without any sign of a structure correlated with the radio halo tail. The temperature of the intracluster medium surrounding IC 310 declines as a function of distance from the cluster center, from kT ∼6keV in the northeast corner of the field of view to about 3keV in the southwest region. Although we do not find any sharp edges in the surface brightness profile, a brightness excess of about 20% over a smooth β model is seen. The temperature also rises by about 10% in the same region. This indicates that the IC 310 region is a subcluster probably infalling into the Perseus cluster, and the gas in front of IC 310 towards the Perseus cluster is likely to be compressed by the large-scale motion, which supports the view that the IC 310 system is undergoing a merger.