星系团之间的大合并可以在团内介质中产生大的湍流和整体流速，从而在重离子的X射线光谱发射线中留下诊断特征。正如Hitomi在对英仙座星系团的观测中所展示的那样，通过高分辨率X射线光谱测量星系团中的气体速度将可以通过即将到来的X射线量热仪来实现，比如XRISM，Athena或Lynx任务。我们调查这种可能性，通过X射线合成光谱与几个电子伏特的能量分辨率的流体动力学模拟的一个主要集群合并的有趣的位置。我们从垂直于合并平面和沿着合并轴的方向观察系统。在这些极端的几何构型中，我们发现了6.7keV铁类氦K_α线的明显的非高斯形状。从模拟中预测的速度色散可以用XRISM Resolve针对最亮的100 ks点进行检索，尽管与复杂的非高斯线形状有关的一些差异。然而，微弱区域的测量需要高S/N，因此需要Athena X-IFU量热计的更大收集面积。与后者，我们还调查了气体的温度和速度梯度跨合并弓形激波边缘，从20”宽的环从一个单一的1 Ms X-IFU指向提取。我们发现最适合的温度和速度色散值，是一致的预测从模拟1西格玛内，但推断的速度色散的不确定性太大，把任何严格的约束浅梯度下游的冲击。我们还提出了模拟图像的热和动力学Sunyaev-Zeldovich的影响，使用上述观察配置，并比较适合未来的天文台，如CMB-S4和AtLAST的角分辨率的结果。
英文摘要：
Major mergers between galaxy clusters can produce large turbulent and bulk flow velocities in the intra-cluster medium and thus imprint diagnostic features in X-ray spectral emission lines from heavy ions. As demonstrated by Hitomi in observations of the Perseus cluster, measurements of gas velocities in clusters from high-resolution X-ray spectra will be achievable with upcoming X-ray calorimeters like those on board XRISM, Athena, or a Lynx like mission. We investigate this possibility for interesting locations across a major cluster merger from a hydrodynamical simulation, via X-ray synthetic spectra with a few eV energy resolution. We observe the system from directions perpendicular to the plane of the merger and along the merger axis. In these extreme geometrical configurations, we find clear non-Gaussian shapes of the iron He-like K_alpha line at 6.7keV. The velocity dispersion predicted from the simulations can be retrieved for the brightest 100ks pointings with XRISM Resolve, despite some discrepancy related to the complex non-Gaussian line shapes. Measurements in faint regions require however high S/N and the larger collecting area of the Athena X-IFU calorimeter is thus needed. With the latter, we also investigate the gas temperature and velocity gradient across the merger bow shock edge, from 20"-wide annuli extracted from a single 1Ms X-IFU pointing. We find best-fit temperature and velocity dispersion values that are consistent with predictions from the simulations within 1-sigma, but the uncertainties on the inferred velocity dispersion are too large to place any stringent constraints on the shallow gradient downstream of the shock. We also present simulated images of the thermal and kinetic Sunyaev-Zeldovich effects, using the above viewing configurations, and compare the results at angular resolutions appropriate for future observatories such as CMB-S4 and AtLAST.
Unveiling the (in)consistencies among the galaxy stellar mass function, star formation histories, satellite abundances and intracluster light from a semi-empirical perspective
Discovery of a nearby radio relic in the low-mass, merging cluster Abell 4067
University of the Witwatersrand（威特沃特斯兰德大学）；University of Pretoria（比勒陀利亚大学）；SKA Observatory（平方公里阵列射电望远镜天文台）；University of Oxford（牛津大学）；Rhodes University（罗兹大学）；South African Radio Astronomy Observatory（南非射电天文观测站）；Texas A&M University（德克萨斯农工大学）；Chulalongkorn University（朱拉隆功大学）
The birth of the intracluster medium: the evolution of multiphase gas and Lyman-$α$ haloes in a simulated $z\sim3$ protocluster
University of Nottingham（诺丁汉大学）；The University of Texas at Dallas（德克萨斯大学达拉斯分校）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；University of Cambridge（剑桥大学）
TNGC-SIDM I: Evolution of massive cluster mergers under the self-interacting dark matter paradigm
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Yonsei University（延世大学）；Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文中心）；Universität Heidelberg（海德堡大学）；University of California, Davis（加州大学戴维斯分校）；Alma Mater Studiorum Università di Bologna（博洛尼亚大学）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天文物理研究所博洛尼亚空间科学与天文观测台）；INFN-Sezione di Bologna（意大利国家核物理研究所博洛尼亚分部）；Massachusetts Institute of Technology（麻省理工学院）；Philipps Universität Marburg（马尔堡菲利普斯大学）
Weak-lensing Analysis of Intracluster Filaments in Abell 2744: Matched-filter Scans and Stepwise 2D Tracing
Yonsei University（延世大学）；California Institute of Technology（加州理工学院）；University of California, Davis（加州大学戴维斯分校）；INAF–Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）
Magnetic fields in the intracluster medium with TNG-Cluster: properties, morphology, and tangential anisotropy
Universität Heidelberg, Zentrum für Astronomie（海德堡大学天文学中心）；Universität Heidelberg, Interdisziplinäres Zentrum für Wissenschaftliches Rechnen（海德堡大学跨学科科学计算中心）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Centre de recherche en astrophysique du Quebec (CRAQ)（魁北克天体物理学研究中心）
From Observations to Simulations: A Neural-Network Approach to Intracluster Medium Kinematics
Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理研究所）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密森天体物理中心）；Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK（剑桥大学天文研究所）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学前沿天文与天体物理研究所）；INAF - IASF Palermo（意大利国家天体物理研究所巴勒莫分部）；Department of Physics and Astronomy, University of Alabama in Huntsville（阿拉巴马大学亨茨维尔分校物理与天文学系）
The merger history of the complex cluster Abell 1758: a combined weak lensing and spectroscopic view
We present a weak-lensing and dynamical study of the complex cluster Abell 1758 (A1758, z = 0.278) supported by hydrodynamical simulations. This cluster is composed of two main structures, called A1758N and A1758S. The Northern structure is composed of A1758NW & A1758NE, with lensing determined masses of 7.90_{-1.55}^{+1.89} X 10^{14} M_ \odot and 5.49_{-1.33}^{+1.67} X 10^{14} M_ \odot , respectively. They show a remarkable feature: while in A1758NW there is a spatial agreement among weak lensing mass distribution, intracluster medium and its brightest cluster galaxy (BCG) in A1758NE the X-ra…
Simulating the impact of dust cooling on the statistical properties of the intracluster medium
从恒星和星系形成的第一阶段开始，非引力过程，如冲压压力剥离、超新星、星系风、活动星系核、星系-星系合并等。导致IGM中的恒星，金属以及尘埃的富集，通过星系物质喷射到IGM中。我们现在知道，这些过程与引力一起形成了结构的形成和演化。我们在这里提出的结构形成的流体动力学模拟实施的效果，由尘埃冷却大尺度结构的形成。我们关注星系团的尺度，研究星系团的统计性质。在这里，我们提出了我们的结果上的$T_X-M$和$L_X-M$标度关系，表现出的斜率和归一化的变化时，由尘埃冷却的标准辐射冷却模型。例如，对于包括尘埃冷却的模型，在$M=10^{14}$ M $_\odot$处，$T_X-M$关系的归一化仅改变最大2%，而在$T_X=1$ keV处，$L_X-T_X$的归一化改变多达10%。我们的研究表明，尘埃是一个额外的非引力过程，有助于塑造热ICM气体的物理状态。
