When the well runs dry: modelling environmental quenching of high-mass satellites in massive clusters at z ≳ 1
When the well runs dry: modelling environmental quenching of high-mass satellites in massive clusters at z ≳ 1
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当井干涸时：对 z ≤ 1 处大质量卫星的环境淬灭进行建模
DOI：
10.1093/mnras/stad2995
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发表时间：
2023
影响因子：
4.8
通讯作者：
Reeves, Andrew M. M.
中科院分区：
文献类型：
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作者：
Baxter, Devontae C.;Cooper, M. C.;Balogh, Michael L.;Rudnick, Gregory H.;De Lucia, Gabriella;Demarco, Ricardo;Finoguenov, Alexis;Forrest, Ben;Muzzin, Adam;Reeves, Andrew M. M.
我们使用MCMC框架探索了大质量星系团atz 101中大质量（> 1010 M）卫星猝灭的模型，重点关注两个主要参数：Rquench（猝灭开始时的主中心半径）和τquench（卫星在穿过Rquench后猝灭的时间尺度）。我们的MCMC分析表明，在一维后验概率分布的Rquenchat约0.25和1.0R200的两个局部最大值。分析四个不同的解决方案，在τquench-Rquenchparameter空间，几乎所有这些产生的静态分数从GOGREEN调查的观测数据相一致，我们调查这些解决方案是否代表不同的淬火途径，并发现它们可以分开的“饥饿”和“核心淬火”的情况。饥饿路径的特征是猝灭时间尺度与中间层的总冷气体（H2+ Hi）耗尽时间尺度大致一致，而核心猝灭的特征是具有相对较高视线速度的卫星在短时间内猝灭到达星系团内部区域（<0.30R200）后的时间尺度（0.25 Gyr）。最后，我们通过比较GOGREEN巡天观测到的过渡星系的性质，打破了这些解之间的简并性。我们的结论是，只有“饥饿”的途径是一致的相空间分布和过渡星系atz 1的相对丰度的投影。然而，我们承认，冲压压力可能有助于作为一个次要的淬火机制。
We explore models of massive (>1010M⊙) satellite quenching in massive clusters atz≳ 1 using an MCMC framework, focusing on two primary parameters:Rquench(the host-centric radius at which quenching begins) and τquench(the time-scale upon which a satellite quenches after crossingRquench). Our MCMC analysis shows two local maxima in the 1D posterior probability distribution ofRquenchat approximately 0.25 and 1.0R200. Analysing four distinct solutions in the τquench–Rquenchparameter space, nearly all of which yield quiescent fractions consistent with observational data from the GOGREEN survey, we investigate whether these solutions represent distinct quenching pathways and find that they can be separated between ‘starvation’ and ‘core quenching’ scenarios. The starvation pathway is characterized by quenching time-scales that are roughly consistent with the total cold gas (H2+ Hi) depletion time-scale at intermediatez, while core quenching is characterized by satellites with relatively high line-of-sight velocities that quench on short time-scales (∼0.25 Gyr) after reaching the inner region of the cluster (<0.30R200). Lastly, we break the degeneracy between these solutions by comparing the observed properties of transition galaxies from the GOGREEN survey. We conclude that only the ‘starvation’ pathway is consistent with the projected phase-space distribution and relative abundance of transition galaxies atz∼ 1. However, we acknowledge that ram pressure might contribute as a secondary quenching mechanism.