发表机构
University of Science and Technology of China; Universidad Autónoma de Madrid; University of Edinburgh; Shanghai Jiao Tong University; Sun Yat-sen University; University of Massachusetts（中国科学技术大学; 马德里自治大学; 爱丁堡大学; 上海交通大学; 中山大学; 马萨诸塞大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文利用ELUCID约束流体模拟，重现后发座星系团的子结构、ICL分布及并合历史，验证了模拟在连接观测与不可观测组装历史中的强大作用。
AI 中文摘要
我们利用ELUCID项目中对后发座星系团的约束流体动力学模拟，研究其子结构与组装历史。我们的模拟准确再现了后发座的整体性质，包括其位置、维里质量、半径以及周围的大尺度丝状结构。通过结合HBT+SKID方法，我们得到总星系团内光（ICL）比例为12.2%–23.5%，与近期观测一致。质量加权的ICL速度弥散、恒星年龄和铁丰度轮廓总体上与MaNGA测量相符，其块状东西向延展与两个最亮星系团星系（BCGs）的并合历史密切相关。模拟还成功再现了弱透镜探测到的北侧和西侧星系团内丝状结构（ICFs），周围星系群的分布与邻近A2199和A1367星系团的方向对齐。模拟进一步预测了复杂的星系团组装历史，包括在红移z=0.74和0.45处的两次重大并合，以及两个BCGs在当前状态前约0.64 Gyr发生的近心通过。我们的结果表明，约束模拟是将观测到的结构与单个星系团不可观测的组装历史联系起来的有力工具。
英文摘要
We employ constrained hydrodynamic simulations of the Coma galaxy cluster from the ELUCID project to study its substructures and assembly history. Our simulations accurately reproduce the global properties of Coma, including its position, virial mass, radius, and surrounding large-scale filaments. Using a combined HBT+SKID method, we obtain a total intracluster light (ICL) fraction of $12.2\%-23.5\%$, consistent with recent observations. The mass-weighted ICL profiles of velocity dispersion, stellar age, and iron abundance generally agree with MaNGA measurements, and its clumpy east-west elongation is closely linked to the merger history of the two brightest cluster galaxies (BCGs). The simulation also successfully reproduces the north and west intracluster filaments (ICFs) detected by weak lensing, and the surrounding galaxy groups are distributed in alignment with the directions toward the nearby A2199 and A1367 clusters. The simulation further predict a complex cluster assembly history, with two major mergers at $z=0.74$ and $0.45$, and a pericentric passage of the two BCGs occurring $\sim 0.64 \ {\rm Gyr}$ before its current state. Our results demonstrate that constrained simulations are a powerful tool for connecting observed structures to the unobservable assembly histories of individual galaxy clusters.
Comments19 pages, 9 figures
