Gas bulk motion in the perseus cluster measured with Suzaku
Gas bulk motion in the perseus cluster measured with Suzaku
复制标题
DOI：
10.1088/0004-637x/782/1/38
复制
发表时间：
2013-12
期刊：
影响因子：
--
通讯作者：
T. Tamura;N. Yamasaki;R. Iizuka;Y. Fukazawa;K. Hayashida;S. Ueda;K. Matsushita;Kosuke Sato;K. Nakazawa;N. Ota;M. Takizawa
中科院分区：
文献类型：
--
作者：
T. Tamura;N. Yamasaki;R. Iizuka;Y. Fukazawa;K. Hayashida;S. Ueda;K. Matsushita;Kosuke Sato;K. Nakazawa;N. Ota;M. Takizawa
我们提出的结果，从朱雀观测英仙座集群，这是相对接近，最明亮的X射线天空，和一个放松的对象与冷核心。X射线成像光谱仪的多次中心区域曝光和偏移指向覆盖半径20 '-30'内的区域。中心数据被用来评估仪器的能量标度校准的准确性确认约300公里s{sup-1}的空间和时间的变化的仪器。这些深度和良好校准的数据被用来测量星系团内介质的X射线红移。在星系团中心以西2 '-4'（45-90 kpc）处发现了气体体运动的迹象，相对于主系统的径向速度约为-（150-300）km s{sup-1}，这里以前曾发现过X射线过剩和冷锋。没有发现其他速度结构。在50-100 kpc的空间尺度上，在中心200 kpc半径范围内，气体径向速度的变化小于300 km s{sup-1}，而在600 kpc半径范围内的400 kpc尺度上，气体径向速度的变化小于600 km s{sup-1}。这些X射线红移分布的空间比较与光学成员星系的themore »第一次在星系团。基于X射线线宽，这些区域内的气体湍流速度也被限制在1000-3000 km s{sup-1}内。这些结果的气体动力学的核心和更大的规模与集群合并活动进行了讨论，并考虑了未来的潜力，高能量分辨率光谱与ASTRO-H。«少
We present the results from Suzaku observations of the Perseus Cluster, which is relatively close, the brightest in the X-ray sky, and a relaxed object with a cool core. A number of exposures of central regions and offset pointing with the X-ray Imaging Spectrometer cover a region within radii of 20'-30'. The central data are used to evaluate the instrumental energy-scale calibration with accuracy confirmed to within around 300 km s{sup –1} by the spatial and temporal variation of the instruments. These deep and well-calibrated data are used to measure X-ray redshifts of the intracluster medium. A hint of gas bulk motion, with radial velocity of about –(150-300) km s{sup –1} relative to the main system, was found at 2'-4' (45-90 kpc) west of the cluster center, where an X-ray excess and a cold front were found previously. No other velocity structure was discovered. Over spatial scales of 50-100 kpc and within 200 kpc radii of the center, the gas-radial-velocity variation is below 300 km s{sup –1}, while over scales of 400 kpc within 600 kpc radii, the variation is below 600 km s{sup –1}. These X-ray redshift distributions are compared spatially with those of optical member galaxies for themore » first time in galaxy clusters. Based on X-ray line widths, gas turbulent velocities within these regions are also constrained within 1000-3000 km s{sup –1}. These results of gas dynamics in the core and larger scales in association with cluster merger activities are discussed, and the future potential of high-energy resolution spectroscopy with ASTRO-H is considered.« less