论文标题
X-MMM $ - $ newton $和$ chandra $的X射线中的Hercules群集
The Hercules cluster in X-rays with $XMM$-$Newton$ and $Chandra$
论文作者
论文摘要
我们提出了一项详细的X射线研究，对附近的中央子集群（$ z $ \ sim $ 0.0368）大力神集群（Abell 2151），被鉴定为A2151C，显示了双峰结构。一块明亮的热气团块，X射线排放延伸至半径$ r $ \ sim $ 304 kpc和$ l_x = 3.03 _ { - 0.04}^{+0.02} \ times10^{43} $ erg S $^{-1} $ in 0.4 $ - $ 7.0 $ - $ 7.0 $ - $ 7.0 $ - $ 7.0 $ - 1} （A2151C（B））。向东（A2151C（f））看到一个不规则，淡淡和冷却的子胶囊$ r $ $ $ $ $ $ 364 kpc，并且具有$ l_x = 1.13 \ pm {0.02} \ times10^{43} {43} $ erg s $^S $^{ - 1} $ 0.4 $ -7.0 $ 7.0 kev。 A2151C（b）的平均温度和元素丰度分别为$ 2.01 \ pm {0.05} $ keV和$ 0.43 \ pm {0.05} $ z $ _ {\ odot} $ z $ _ {\ odot} $用于A2151C（F）。低温（$ {1.55} \ pm {0.07} $ keV）和中央15 Arcsec区域内的短冷却时间（$ \ sim $ 0.81 Gyr）确认在A2151C（B）中存在冷核。我们在A2151C（F）中识别几个紧凑的星系组。我们发现，在形成过程中，A2151C（F）是一个独特的星系组，并且可能不是大力神（A2151E）的东部子集群的一部分的RAM压力。来自A2151C的X射线发射显示了A2151C（B）和A2151C（F）之间的重叠区域，但在二维（2D）投影的热力学图中的温度或熵没有任何增强的区域，这可能表明由于两个亚趋势之间的合并而导致的相互作用。
We present a detailed X-ray study of the central subcluster of the nearby ($z$ $\sim$0.0368) Hercules cluster (Abell 2151) identified as A2151C that shows a bimodal structure. A bright clump of hot gas with X-ray emission extending to radius $r$ $\sim$304 kpc and $L_X = 3.03_{-0.04}^{+0.02}\times10^{43}$ erg s$^{-1}$ in the 0.4$-$7.0 keV energy range is seen as a fairly regular subclump towards the west (A2151C(B)). An irregular, fainter and cooler subclump with radius $r$ $\sim$364 kpc is seen towards the east (A2151C(F)) and has $L_X=1.13\pm{0.02}\times10^{43}$ erg s$^{-1}$ in the 0.4$-$7.0 keV energy band. The average temperature and elemental abundance of A2151C(B) are $2.01\pm{0.05}$ keV and $0.43\pm{0.05}$ Z$_{\odot}$ respectively, while these values are $1.17\pm{0.04}$ keV and $0.13\pm{0.02}$ Z$_{\odot}$ for A2151C(F). Low temperature (${1.55}\pm{0.07}$ keV) and a short cooling time ($\sim$0.81 Gyr) within the central 15 arcsec region confirm the presence of a cool core in A2151C(B). We identify several compact groups of galaxies within A2151C(F). We find that A2151C(F) is a distinct galaxy group in the process of formation and likely not a ram-pressure stripped part of the eastern subcluster in Hercules (A2151E). X-ray emission from A2151C shows a region of overlap between A2151C(B) and A2151C(F) but without any enhancement of temperature or entropy in the two-dimensional (2D) projected thermodynamic maps that could have indicated an interaction due to merger between the two subclumps.
