Detection of anisotropic satellite quenching in galaxy clusters up to z ∼ 1
Detection of anisotropic satellite quenching in galaxy clusters up to z ∼ 1
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DOI：
10.1093/mnras/stac3251
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发表时间：
2022-08
影响因子：
4.8
通讯作者：
M. Ando;K. Shimasaku;Kei Ito
中科院分区：
文献类型：
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作者：
M. Ando;K. Shimasaku;Kei Ito
星团环境中的卫星星系比一般星团环境中的星系更容易被淬灭。最近，有报道称卫星星系的猝灭取决于相对于其中心星系的方向：沿中心长轴的卫星比沿小轴的卫星更容易猝灭。在本文中，我们报告了基于Hyper prime- cam Subaru战略计划构建的大型光学选择簇目录对高达z ～ 1的这种各向异性淬火的检测。我们计算了静止卫星星系分数作为从中心星系长轴测得的取向角的函数，发现静止卫星星系分数在0.25 r200m处。我们还证实，观测到的各向异性不能用局部星系密度或沿两个轴的恒星质量分布的差异来解释。两个轴之间的静态分数过剩表明，导致各向异性的淬火效率几乎与恒星质量无关，至少低于我们的恒星质量极限$M_{*}=1\times 10^{10}\, {\rm M}_{\odot }$。最后，我们认为观测到的各向异性的物理起源应该具有比$\sim 1\, \mathrm{Gyr}$更短的淬火时间尺度，如冲压压力剥离，因为要观测到各向异性淬火，卫星必须在其初始取向角发生显著变化之前进行淬火。
Satellite galaxies in the cluster environment are more likely to be quenched than galaxies in the general field. Recently, it has been reported that satellite galaxy quenching depends on the orientation relative to their central galaxies: satellites along the major axis of centrals are more likely to be quenched than those along the minor axis. In this paper, we report a detection of such anisotropic quenching up to z ∼ 1 based on a large optically selected cluster catalogue constructed from the Hyper Suprime-Cam Subaru Strategic Program. We calculate the quiescent satellite galaxy fraction as a function of orientation angle measured from the major axis of central galaxies and find that the quiescent fractions at 0.25 r200m). We also confirm that the observed anisotropy cannot be explained by differences in local galaxy density or stellar mass distribution along the two axes. Quiescent fraction excesses between the two axes suggest that the quenching efficiency contributing to the anisotropy is almost independent of stellar mass, at least down to our stellar mass limit of $M_{*}=1\times 10^{10}\, {\rm M}_{\odot }$. Finally, we argue that the physical origins of the observed anisotropy should have shorter quenching time-scales than $\sim 1\, \mathrm{Gyr}$, like ram-pressure stripping, because, for anisotropic quenching to be observed, satellites must be quenched before their initial orientation angles are significantly changed.