The localization of galaxy groups in close proximity to galaxy clusters using cosmic web nodes
The localization of galaxy groups in close proximity to galaxy clusters using cosmic web nodes
复制标题
使用宇宙网节点定位靠近星系团的星系群
DOI：
10.1093/mnras/stad3205
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发表时间：
2024
影响因子：
4.8
通讯作者：
Cornwell D
中科院分区：
文献类型：
--
作者：
Cornwell D
我们研究了使用 DisPerSE 拓扑细丝探测器识别的宇宙网节点来系统地识别大质量星团周围的坠落区域中的星系群的有效性。星系团周围区域的星系的大随机运动和坠落速度使通过正常的群发现算法检测和表征子结构变得复杂。然而，了解细丝和/或星系群内星系的共置是了解环境对星系演化的作用的关键部分，特别是考虑到下一代广视场光谱调查。在这里，我们使用来自 TheThreeHundred 合作的模拟大型星团，并将派生的群目录（σv> 300h−1km s−1 的光环）与 DisPerSE 的临界点进行比较，在超过 100 个粒子的光环上运行。我们发现，在 3D 中，56% 的 DisPerSE 节点被正确识别为组（纯度），而 68% 的组被识别为节点（完整性）。匹配的比例随着群体质量和与宿主集群中心的距离的增加而增加。对于 3D 中质量最大的星系群 (M> 1014M⊙)，完整性达到 100%；考虑到预计的 2D 星系分布，完整性达到 63%。当宇宙网节点和星系群之间发生完美匹配时，DisPerSE 节点密度 (δ) 可以作为该群质量的估计值，尽管分散程度很大。我们的结论是，宇宙细丝探测器的使用有望成为一种有用且直接的观测工具，用于解开大质量星团坠落区域内的子结构。
We investigate the efficacy of using the cosmic web nodes identified by the DisPerSE topological filament finder to systematically identify galaxy groups in the infall regions around massive clusters. The large random motions and infall velocities of galaxies in the regions around clusters complicate the detection and characterisation of substructures through normal group-finding algorithms. Yet understanding the co-location of galaxies within filaments and/or groups is a key part of understanding the role of environment on galaxy evolution, particularly in light of next-generation wide-field spectroscopic surveys. Here we use simulated massive clusters from TheThreeHundred collaboration and compare the derived group catalogues, (haloes with σv> 300h−1km s−1) with the critical points from DisPerSE, ran on haloes with more than 100 particles. We find that in 3D, 56 per cent of DisPerSE nodes are correctly identified as groups (purity) while 68 per cent of groups are identified as nodes (completeness). The fraction of matches increases with group mass and with distance from the host cluster centre. This rises to a completeness of 100 per cent for the most massive galaxy groups (M> 1014M⊙) in 3D, or 63 per cent when considering the projected 2D galaxy distribution. When a perfect match occurs between a cosmic web node and a galaxy group, the DisPerSE node density (δ) serves as an estimate of the group’s mass, albeit with significant scatter. We conclude that the use of a cosmic filament finder shows promise as a useful and straightforward observational tool for disentangling substructure within the infall regions of massive clusters.