发表机构
Graduate School of Science, Nagoya University; Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University; NASA / Goddard Space Flight Center; Department of Astronomy, University of Geneva; Department of Physics, Tokyo Metropolitan University; RIKEN Nishina Center; Graduate School of Advanced Science and Engineering, Hiroshima University（名古屋大学理学研究科; 名古屋大学小林益川粒子宇宙起源研究所; 美国国家航空航天局戈达德太空飞行中心; 日内瓦大学天文学系; 东京都立大学物理学系; 理化学研究所西村中心; 广岛大学先进理工学研究科）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
通过XRISM对后发星系团核心X射线发射线轮廓的详细分析，发现了新的蓝移和红移速度成分，并估计ICM湍流与整体运动能量密度相当且数倍于磁场能量密度。
AI 中文摘要
合并中的星系团其星系团内介质（ICM）表现出湍流和整体流动。揭示这些成分不仅对于阐明星系团合并的几何结构至关重要，而且对于理解磁场放大和相对论性粒子加速的物理机制也至关重要。XRISM/Resolve对后发星系团核心两个$3'\times3'$天区的数据揭示，中心天区内的ICM相对于星系团星系平均速度以$\Delta cz = -430$ km s$^{-1}$运动，而南部天区则以$\Delta cz = -730$ km s$^{-1}$运动（见\cite{2025ApJ...985L..20X}，以下简称“论文I”）。在本文中，我们对这些数据集进行了更详细的分析，以搜索Fe-K线复合轮廓中的非高斯特征。在中心天区西北（NW）象限的光谱中，除了论文I中报告的主成分和红移ICM成分（$\Delta cz = -40$ km s$^{-1}$）外，我们还发现了另一个蓝移成分的证据，其运动速度为$\Delta cz = -1250$ km s$^{-1}$。为了系统地搜索其他显著的速度成分，我们对来自中心天区和南部天区的Resolve全阵列光谱进行了无偏的3 eV步长多成分拟合。这一搜索在南部天区发现了另一个红移成分，其运动速度为$\Delta cz \sim +1230$ km s$^{-1}$。我们估计ICM湍流和整体运动的能量密度彼此相近，并且是星系团$B\sim 5~\mu$G磁场能量密度的数倍。
英文摘要
The intracluster medium (ICM) in merging galaxy clusters exhibits turbulence and bulk flows. Unraveling these components is crucial not only for elucidating the geometry of the cluster mergers, but also for understanding the physics of magnetic field amplification and relativistic particle acceleration. XRISM/Resolve data for two $3'\times3'$ fields in the core of the Coma cluster reveales that the ICM in the central field moves with $Δcz = -430$~km~s$^{-1}$ relative to the cluster galaxy average, while that in the southern field moves with $Δcz = -730$~km~s$^{-1}$ (see \cite{2025ApJ...985L..20X}, hereinafter ``Paper I''). In this paper, we perform a more detailed analysis of these data sets to search for non-Gaussian features in the Fe-K line complex profiles. In the spectra from the northwest (NW) quadrant of the central field, in addition to the main and redshifted ICM components ($Δcz = -40$ km s$^{-1}$) reported in Paper I, we find evidence of another, blueshifted component, moving with $Δcz = -1250$ km s$^{-1}$. For a systematic search for other significant velocity components, we perform a bias-free 3 eV step multi-component fit to the Resolve full-array spectra from the central and southern fields. This search uncovers another redshifted component in the southern field, moving with $Δcz \sim +1230$ km s$^{-1}$. We estimate the energy densities of the ICM turbulence and bulk motion to be similar to each other and several times greater than the energy density of the cluster's $B\sim 5~μ$G magnetic field.
Comments9 pages, 5 figure, PASJ accepted
