近日，XRISM国际协作组Elena Bellomi团队研究了英仙座星系团中多个气体运动驱动因子。相关论文于2026年1月28日发表在《自然》杂志上。

星系团作为宇宙中最大的晕结构，其内部充满温度介于1000万至1亿度的X射线辐射气体。星系团的演化受到超大质量黑洞反馈和与其他宇宙结构合并等高能过程的塑造，但这些过程在气体运动学上留下的痕迹迄今仍不明确，限制了人们对星系团内部能量转换机制的理解。XRISM天文台的高分辨率光谱测绘为此提供了突破路径。

研究组基于XRISM对英仙座星系团冷核区域径向延展的运动学测量，首次发现至少存在两种主导气体运动的驱动源：其一小尺度驱动源位于星系团内部约60千秒差距范围内，很可能与超大质量黑洞的反馈活动相关；其二大尺度驱动源作用于外核区域，由星系团合并过程提供能量。

这一发现表明，在黑洞活跃阶段，超大质量黑洞的反馈机制能够驱动气体运动。若这些运动能量完全耗散为热能，将可能在抵消英仙座星系团核心区域辐射冷却损失方面发挥重要作用。研究组强调了开展延展源运动学测绘观测的必要性，以准确刻画星系团的物质速度场及其在质量晕演化中的作用，并为超大质量黑洞反馈模型提供了运动学诊断方法。

附：英文原文

Title: Disentangling multiple gas kinematic drivers in the Perseus galaxy cluster

Author: Congyao Zhang, Annie Heinrich, Irina Zhuravleva or Elena Bellomi.

Issue&Volume: 2026-01-28

Abstract: Galaxy clusters, the Universe’s largest halo structures, are filled with an X-ray-emitting gas with a temperature between 10million and 100million degrees. Their evolution is shaped by energetic processes such as feedback from supermassive black holes (SMBHs) and mergers with other cosmic structures1,2,3. The imprints of these processes on gas kinematics remain largely unknown, restricting our understanding of energy conversion within clusters4. High-resolution spectral mapping with the X-Ray Imaging and Spectroscopy Mission (XRISM) observatory5 offers a way forward6,7. Here we present XRISM kinematic measurements of the Perseus cluster, radially covering the extent of its cool core. We find direct evidence for at least two dominant drivers of gas motions operating on distinct physical scales: a small-scale driver in the inner approximately 60kpc, probably associated with the SMBH feedback; and a large-scale driver in the outer core, powered by mergers. This finding suggests that, during the active phase, SMBH feedback drives gas motions, which, if fully dissipated into heat, could have a substantial role in offsetting radiative cooling losses in the Perseus core. Our study underscores the necessity of kinematic mapping observations of extended sources to robustly characterize the velocity fields and their role in the evolution of massive halos. It further offers a kinematic diagnostic for SMBH feedback models.

DOI: 10.1038/s41586-025-10017-x

Source: https://www.nature.com/articles/s41586-025-10017-x