Non-thermal X-rays, a high-abundance ridge and fossil bubbles in the core of the Perseus cluster of galaxies
Non-thermal X-rays, a high-abundance ridge and fossil bubbles in the core of the Perseus cluster of galaxies
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DOI：
10.1111/j.1365-2966.2005.09016.x
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发表时间：
2005-03
影响因子：
4.8
通讯作者：
J. Sanders;A. Fabian;R. Dunn
中科院分区：
文献类型：
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作者：
J. Sanders;A. Fabian;R. Dunn
利用钱德拉对英仙座星系团的深层观测，我们发现了一个距离中央核250弧秒（93千秒差距）的高丰度壳层。这个山脊位于英仙座无线电迷你光环的边缘。此外，我们确定两个哈丝指向这个壳。我们假设这个脊是一个化石射电泡的边缘，由从星团核心升起的夹带富集物质形成。壳外有温度跃变，但压力是连续的，表明有冷锋。一个非热的组件映射在集群的核心与形态类似的迷你晕。它的总光度为4.8 × 1043 ergs-1，半径为1075 kpc。假设非热辐射是宇宙微波背景辐射和NGC 1275红外辐射的逆康普顿散射的结果，我们绘制了星系团核心的磁场。
Using a deep Chandra observation of the Perseus cluster of galaxies, we find a high-abundance shell 250 arcsec (93 kpc) from the central nucleus. This ridge lies at the edge of the Perseus radio mini-halo. In addition we identify two Ha filaments pointing towards this shell. We hypothesize that this ridge is the edge of a fossil radio bubble, formed by entrained enriched material lifted from the core of the cluster. There is a temperature jump outside the shell, but the pressure is continuous indicating a cold front. A non-thermal component is mapped over the core of the cluster with a morphology similar to the mini-halo. Its total luminosity is 4.8 × 10 43 erg s -1 , extending in radius to ∼75 kpc. Assuming the non-thermal emission to be the result of inverse Compton scattering of the cosmic microwave background and infrared emission from NGC 1275, we map the magnetic field over the core of the cluster.