Based mainly on X-ray observations, studies are made on interactions between the intra-cluster medium (ICM) in clusters of galaxies and their member galaxies. Through (magneto)hydrodynamic and gravitational channels, the moving galaxies are expected to drag the ICM around them, and transfer to the ICM some fraction of their dynamical energies on cosmological time scales. This hypothesis is in line with several observations, including the possible cosmological infall of galaxies towards the cluster center, found over redshifts of z~1 to z~0. Further assuming that the energy lost by the galaxies is first converted into ICM turbulence and then dissipated, this picture can explain the subsonic and uniform ICM turbulence, measured with Hitomi in the core region of the Perseus cluster. The scenario may also explain several other unanswered problems regarding clusters of galaxies, including what prevents the ICM from the expected radiative cooling, how the various mass components in nearby clusters have attained different radial distributions, and how a thermal stability is realized between hot and cool ICM components that co-exist around cD galaxies. This view is also considered to pertain to the general scenario of galaxy evolution, including their environmental effects.
What Do the Hitomi Observations Tell Us About the Turbulent Velocities in the Perseus Cluster? Probing the Velocity Field with Mock Observations
Hitomi首次直接测量了英仙座星系团的气体运动，这意味着它的核心相当“静止”，速度小于200 km s $\sim$，尽管存在活动星系核和晃动的冷锋。在以前的工作的基础上，我们使用合成Hitomi/SXS观测模拟集群的热等离子体与晃动的气体运动和不同的粘度，以类似的方式分析其速度结构。我们发现，晃动运动可以产生类似于瞳测量的线位移和宽度。我们发现这些测量不受气体粘度值的影响，因为它的影响只在小于SXS $\sim$ 1' PSF的角标度上清楚地表现出来。PSF使靠近核心的区域的谱线偏移偏置多达$\sim 40-50$ km s $^{-1}$，因此仔细模拟这种效应至关重要。我们还推断，如果晃动的运动占主导地位的观察速度梯度，英仙座必须观察到从这些运动的平面有点倾斜的视线，但仍然允许螺旋图案是可见的。最后，我们发现，假设各向同性的运动可以低估的总速度和动能的核心在我们的模拟多达$\sim$ 60%。然而，在我们模拟的集群核心的总动能仍然是不到10%的热能的核心，与瞳观测。
Turbulence in Simulated Local Cluster Analogs: One-to-one comparisons between SLOW and XRISM/Hitomi
Ludwig-Maximilians-Universität München（慕尼黑路德维希-马克西米利安大学）；Università degli Studi di Trieste（的里雅斯特大学）；INAF - Astronomical Observatory of Trieste（意大利国家天体物理研究所的里雅斯特天文台）；INFN, Instituto Nazionale di Fisica Nucleare（意大利国家核物理研究所）；ICSC - Italian Research Center on High Performance Computing, Big Data and Quantum Computing（意大利高性能计算、大数据和量子计算研究中心）；European Southern Observatory（欧洲南方天文台）；IFPU – Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）
Disentangling AGN Feedback and Sloshing in the Perseus Cluster with XRISM: Insights from Simulations
University of Maryland, Baltimore County (UMBC)（马里兰大学巴尔的摩分校）；NASA / Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；University of Chicago（芝加哥大学）；Masaryk University（马萨里克大学）；University of Michigan（密歇根大学）；University of Waterloo（滑铁卢大学）；Université de Montréal（蒙特利尔大学）；Centre de recherche en astrophysique du Québec (CRAQ)（魁北克天体物理研究中心）
Chemical enrichment in the Ophiuchus cluster core studied by high-resolution XRISM spectroscopy
Institute of Space and Astronautical Science, JAXA（宇宙科学研究所）；Department of Physics, Tokyo Metropolitan University（东京都立大学物理系）；Department of Astrophysics and Atmospheric Sciences, Kyoto Sangyo University（京都产业大学天体物理学与大气科学系）；Department of Physics, Hiroshima University（广岛大学物理系）；Department of Physics, Saitama University（埼玉大学物理系）
利用高分辨率XRISM光谱学研究Ophiuchus团核心的化学富集，发现其X/Fe比值与太阳一致，通过核心坍缩和Ia型超新星模型解释丰度模式，揭示Ca的不足可能由Ca-rich gap transients贡献。
c-C3H2 deuteration towards prestellar and starless cores in the Perseus Molecular Cloud
RIKEN Cluster for Pioneering Research（理化学研究所前沿研究集群）；National Radio Astronomy Observatory（国家射电天文台）；University of Virginia（弗吉尼亚大学）；University of California, Berkeley（加州大学伯克利分校）；University of Arizona（亚利桑那大学）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙高等科学研究委员会-国家航空航天技术研究所）
Diffuse Dwarf Galaxies in Galaxy Clusters: I. Stellar Populations and Radial Gradients
Center for Astrophysics and Supercomputing, Swinburne University（斯威本大学天体物理学与超级计算中心）；Department of Physics and Astronomy, San José State University（圣何塞州立大学物理与天文系）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Departamento de Astrofísica, Universidad de La Laguna（拉帕尔马大学天体物理学系）；Department of Astronomy and Astrophysics, University of California Santa Cruz（加州大学圣克鲁兹分校天文与天体物理学系）
