CODEX: Role of velocity substructure in the scaling relations of galaxy clusters
CODEX: Role of velocity substructure in the scaling relations of galaxy clusters
复制标题
CODEX：速度子结构在星系团尺度关系中的作用
DOI：
10.1051/0004-6361/202245308
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发表时间：
2023
影响因子：
6.5
通讯作者：
Damsted S
中科院分区：
文献类型：
--
作者：
Damsted S
星系团作为宇宙探测器的使用依赖于对其性质的详细了解。他们定义了与宇宙意义上重要的群集质量函数相关的群集选择和排序。以往的研究采用小样本的团簇，集中于实现团簇性质与质量的第一次校准，而通过详细的研究揭示了团簇性质的多样性。目的：利用SDSS和NOT对CODEX聚类样本进行大规模光谱跟踪，可以对数百个聚类进行详细研究，从而消除以前样本的局限性。我们的目标是通过对后续光谱结果运行光谱群查找器，并将簇的动态状态与其标度关系联系起来，更新CODEX的光谱簇识别。方法基于redMaPPer隶属度，采用可重复的光谱隶属度测定和清洗程序，对后续的光谱结果运行光谱组查找器，对光谱异常值进行隶属度清洗。我们对速度子结构进行了安德森-达令检验，并分析了它对标度关系的影响。我们还测试了x光中心偏移对缩放关系的影响。结果我们报告了至少有15个成员的完整星团样本的丰富度、x射线光度和速度色散之间的标度关系。对于给定丰富度，具有速度子结构的簇表现出增强的速度散度，其特征是散度大2.5倍。在x射线-光学中心具有强偏移的团簇与具有子结构的团簇具有可比的缩放关系。我们证明了低丰度星系团和高丰度星系团的尺度关系参数具有一致性。通过红移分割簇，我们注意到在所有缩放关系中，随着红移的增加，散点减少。我们将观测到高散射的红移范围定位为z< 0.15，这与文献中关于散射的结果一致。我们注意到高光度星团和低光度星团的散射增加isz< 0.15，这表明冷却和由此产生的活动星系核反馈是这种散射的根源。
ContextThe use of galaxy clusters as cosmological probes relies on a detailed understanding of their properties. They define cluster selection and ranking linked to a cosmologically significant cluster mass function. Previous studies have employed small samples of clusters, concentrating on achieving the first calibrations of cluster properties with mass, while the diversity of cluster properties has been revealed via detailed studies.AimsThe large spectroscopic follow-up on the CODEX cluster sample with SDSS and NOT enables a detailed study of hundreds of clusters, lifting the limitations of previous samples. We aim to update the spectroscopic cluster identification of CODEX by running the spectroscopic group finder on the follow-up spectroscopy results and connecting the dynamical state of clusters to their scaling relations.MethodsWe implemented a reproducible spectroscopic membership determination and cleaning procedures, based on the redMaPPer membership, running the spectroscopic group finder on the follow-up spectroscopy results and cleaning the membership for spectroscopic outliers. We applied the Anderson-Darling test for velocity substructure and analysed its influence on the scaling relations. We also tested the effect of the X-ray-to-optical centre offset on the scaling relations.ResultsWe report on the scaling relations between richness, X-ray luminosity, and velocity dispersion for a complete sample of clusters with at least 15 members. Clusters with velocity substructure exhibit enhanced velocity dispersion for a given richness and are characterized by 2.5 times larger scatter. Clusters that have a strong offset in X-ray-to-optical centres have comparable scaling relations as clusters with substructure. We demonstrate that there is a consistency in the parameters of the scaling relations for the low- and high-richness galaxy clusters. Splitting the clusters by redshift, we note a decrease in scatter with redshift in all scaling relations. We localize the redshift range where a high scatter is observed toz< 0.15, which is in agreement with the literature results on the scatter. We note that the increase in scatter for both high- and low-luminosity clusters isz< 0.15, suggesting that both cooling and the resulting active galactic nucleus feedback are at the root of this scatter.