MKW 3s内的降雨：3CR 318.1周围X射线冷灯丝的Chandra-MUSE分析
Raining in MKW 3s: a Chandra-MUSE analysis of X-ray cold filaments around 3CR 318.1
摘要：
本文分析了在与MKW 3s的一个冷核星系团的布里渊星系团（BCG）NGC 5920有关的射电源3CR 318.1中观测到的气体细丝的X射线和光学观测结果。这项工作是第一个X射线和光学分析的细丝在冷核心集群进行使用MUSE观测。我们的目标是确定主要的激发过程负责从这些灯丝所产生的排放。我们用X射线$\textit{Chandra}$观测较热的高度电离的气相，补充了光学VLT/MUSE观测，追踪较冷的气相。使用MUSE观测，我们研究了沿灯丝的发射线强度比，以约束驱动激发的物理过程，并且使用$\textit{Chandra}$观测，我们对沿这些灯丝的气体进行了光谱分析。我们发现了这些细丝的X射线和光学形态之间的空间关联，这些细丝比周围的团簇内介质（ICM）更冷，金属丰度更低，正如在其他BCGs中已经看到的那样。与以前的结果相比，从文献中的其他BCGs，我们建议，激发过程，这是最有可能负责这些灯丝发射是恒星形成和冲击的组合，与自电离，冷却ICM可能的贡献。此外，我们得出结论，细丝最有可能起源于活动星系核驱动的流出方向的无线电喷流。
英文摘要：
We present the analysis of X-ray and optical observations of gas filaments observed in the radio source 3CR 318.1, associated with NGC 5920, the Brightest Cluster Galaxy (BCG) of MKW 3s, a nearby cool core galaxy cluster. This work is one of the first X-ray and optical analyses of filaments in cool core clusters carried out using MUSE observations. We aim at identifying the main excitation processes responsible for the emission arising from these filaments. We complemented the optical VLT/MUSE observations, tracing the colder gas phase, with X-ray $\textit{Chandra}$ observations of the hotter highly ionized gas phase. Using the MUSE observations, we studied the emission line intensity ratios along the filaments to constrain the physical processes driving the excitation, and, using the $\textit{Chandra}$ observations, we carried out a spectral analysis of the gas along these filaments. We found a spatial association between the X-ray and optical morphology of these filaments, which are colder and have lower metal abundance than the surrounding intra-cluster medium (ICM), as already seen in other BCGs. Comparing with previous results from the literature for other BCGs, we propose that the excitation process that is most likely responsible for these filaments emission is a combination of star formation and shocks, with a likely contribution from self-ionizing, cooling ICM. Additionally, we conclude that the filaments most likely originated from AGN-driven outflows in the direction of the radio jet.
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