We present a detailed analysis of two merging clusters, from XMM-\textit{Newton} X-ray archival data: PLCKESZ G036.7+14.9 ($z=0.15$; hereafter G036) and PLCK G292.5+22.0 ($z=0.30$; hereafter G292). We notice that the intracluster medium is heated as a result of the merger, and we find evidence for a merger shock in the region between both subcluster haloes. X-ray observations confirm that the shocks in these systems are among the hottest known in the literature. From the ICM analysis of temperature discontinuity, the Mach numbers were determined to be $M_{\rm G036}=1.3$ and $M_{\rm G292}=1.5$ for G036 and G292, respectively. In this paper, for each cluster, we propose a hydrodynamic model for the merger as a whole, compatible with their diffuse X-ray emission and temperature maps. The simulations suggest that both clusters are observed shortly before pericentric passage. Our simulation results indicate that the merger of the G036 system is seen at an inclination of 50$^{\circ}$ (the angle between the plane of the orbit and the plane of the sky), and merely 50 Myr prior to the pericentric passage. In the case of G292, the subclusters would be merging not far from the plane of the sky ($i=18^{\circ}$) and are observed 150\,Myr before the two cores collide.
Spectroscopic galaxy redshifts in the Peanut cluster -- a massive nearly head-on cluster merger shortly after pericenter passage
Space Research Institute (IKI), Russian Academy of Sciences（俄罗斯科学院空间研究所）；Kazan Federal University (KFU)（喀山联邦大学）；Tatarstan Academy of Sciences（鞑靼斯坦共和国科学院）；Special Astrophysical Observatory (SAO), Russian Academy of Sciences（俄罗斯科学院特殊天文台）；Max Planck Institute for Astrophysics (MPA)（马克斯·普朗克天体物理研究所）；Institute of Applied Astronomy (IAA), Russian Academy of Sciences（俄罗斯科学院应用天文研究所）
Interacting galaxies on FIRE-2: The connection between enhanced star formation and interstellar gas content
我们提出了一套全面的高分辨率（秒差距尺度），理想化的（非宇宙学）星系合并模拟（24轮，恒星质量比~2.5：1），以研究相互作用引起的恒星形成和星际介质（ISM）在各种温度密度制度的演变之间的联系。我们使用GIZMO代码和第二版的“真实环境中的反馈”模型（FIRE-2），该模型捕获了ISM的多阶段结构。我们的模拟旨在代表本地宇宙中的星系合并。在这项工作中，我们专注于“星系对周期”之间的第一次和第二次近心轴通道。我们分裂的ISM分为四个制度：热，温暖，冷，冷密集，热，电离，原子和分子的气体在真实星系中观察到的阶段的动机。我们发现，平均而言，相互作用提高了这对恒星的形成率（约30%，合并套件样本平均值），并提高了它们的冷致密气体含量（约18%）。这伴随着热气体的减少（~11%），冷气体的变化可以忽略不计（~4%的增加），以及热气体的大幅增加（~400%）。密度超过1000 cm ^3的冷密气体（冷超密区）的数量显著增加（约240%），但仅占冷密气体预算的0.15%（平均）。
Weak lensing and spectroscopic analysis of the nearby dissociative merging galaxy cluster Abell 3376
The galaxy cluster Abell~3376 is a nearby (z=0.046) dissociative merging cluster surrounded by two prominent radio relics and showing an X-ray comet-like morphology. The merger system is comprised of the subclusters A3376W & A3376E. Based on new deep multi-wavelength large-field images and published redshifts, we bring new insights about the history of this merger. Despite the difficulty of applying the weak lensing technique at such low redshift, we successfully recovered the mass distribution in the cluster field. Moreover, with the application of a two-body model, we have addressed the dyna…
The Merger Dynamics of the Galaxy Cluster Abell 1775: New Insights from Chandra and XMM-Newton for a Cluster Simultaneously Hosting a WAT and a NAT Radio Sources
ELUCID. IX. Recovering the Substructures and History of the Coma Cluster
University of Science and Technology of China（中国科学技术大学）；Universidad Autónoma de Madrid（马德里自治大学）；University of Edinburgh（爱丁堡大学）；Shanghai Jiao Tong University（上海交通大学）；Sun Yat-sen University（中山大学）；University of Massachusetts（马萨诸塞大学）
The extreme Disturbed Galaxy Cluster Sample (eDGeS): Spectroscopy and Dynamical Analysis of the eROSITA-Selected Merging Galaxy Cluster Candidate 1eRASS J025859.4-193727
University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）；International Gemini Observatory, NSF NOIRLab（国际双子座天文台，NSF NOIRLab）；Cerro Tololo Inter-American Observatory, NSF NOIRLab（塞罗托洛洛美洲际天文台，NSF NOIRLab）；Observatório Nacional (ON/MCTI)（国家天文台（ON/MCTI））；Universidad de La Serena（拉塞雷纳大学）；Max Planck Institute for Extraterrestrial Physics（马普地外物理研究所）
Formation of globular cluster-rich ultra-diffuse galaxies through mergers
International Centre for Radio Astronomy Research, The University of Western Australia（西澳大利亚大学国际无线电天文研究中心）；National Institute of Technology, Asahikawa College（旭川工业高等专门学校）；ATNF, CSIRO Space and Astronomy（CSIRO空间与天文台射电天文国家设施）；Centre for Astrophysics and Supercomputing, Swinburne University（斯威本科技大学天体物理学与超级计算中心）
