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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Suzaku observations of the outskirts of the galaxy cluster Abell 3395, including a filament toward Abell 3391
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Suzaku observations of the outskirts of the galaxy cluster Abell 3395, including a filament toward Abell 3391

机译：Suzaku观察Galaxy集群Abell 3395的郊区，包括朝向Abell 3391的灯丝

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摘要

The results of Suzaku observations of the outskirts of Abell 3395, including a large-scale structure filament toward Abell 3391, are presented. We measured temperature and abundance distributions from the southern outskirt of A3395 to the north at the virial radius, where a filament structure has been found in the former X-ray and Sunyaev-Zel'dovich (SZ) effect observations between A3391 and A3395. The overall temperature structure is consistent with the universal profile proposed by Okabe, N., et al. 2014, PASJ, 66, 99 for relaxed clusters, except for the filament region. A hint of intracluster medium heating is found between the two clusters, which might be due to their interaction in the early phase of a cluster merger. Although we obtained a relatively low metal abundance of Z = 0.169(-0.150-0.004-0.015)(+0.164+0.009+0.018) solar, where the first, second, and third errors are statistical, cosmic X-ray background systematic, and non-X-ray background systematic, respectively, at the virial radius in the filament, our results are still consistent with previous results for other clusters (Z similar to 0.3 solar) within errors. Therefore, our results are also consistent with the early enrichment scenario. We estimated Compton y parameters only from X-ray results in the region between A3391 and A3395 assuming a simple geometry. They are smaller than the previous SZ results with the Planck satellite. The difference could be attributed to a more elaborate geometry such as a filament inclined to the line-of-sight direction, or underestimation of the X-ray temperature because of the unresolved multi-temperature structures or undetected hot X-ray emission of the shock-heated gas.
机译：本文介绍了朱雀对阿贝尔3395郊区的观测结果，包括对阿贝尔3391的大规模结构细丝。我们测量了从A3395南郊到维里半径北部的温度和丰度分布，在先前的X射线和Sunyaev-Zel’dovich（SZ）效应观测中，在A3391和A3395之间发现了细丝结构。整体温度结构与Okabe，N.，et al.2014，PASJ，66，99提出的松弛簇的通用轮廓一致，但灯丝区域除外。在两个团簇之间发现了团簇内介质加热的迹象，这可能是由于它们在团簇合并的早期阶段相互作用的结果。虽然我们获得了相对较低的金属丰度Z=0.169（-0.150-0.004-0.015）（+0.164+0.009+0.018）太阳，其中第一、第二和第三个误差分别是统计误差、宇宙X射线背景系统误差和非X射线背景系统误差，在灯丝的维里半径处，我们的结果在误差范围内仍然与其他星团（Z类似于0.3太阳）的先前结果一致。因此，我们的结果也与早期浓缩情景一致。我们仅根据A3391和A3395之间区域的X射线结果估计康普顿y参数，假设几何结构简单。它们比之前普朗克卫星的SZ结果要小。这种差异可归因于更精细的几何结构，如一根向视线方向倾斜的灯丝，或由于未分辨的多温度结构或未检测到的冲击加热气体的热X射线发射，而低估了X射线温度。

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