The hot circumgalactic media of massive cluster satellites in the TNG-Cluster simulation: existence and detectability
Eric Rohr, Annalisa Pillepich, Dylan Nelson, Mohammadreza Ayromlou, Elad Zinger
备注：
Submitted to A&A, comments welcome. See companion papers by Nelson et al., Lehle et al., Truong et al., Lee et al., and Ayromlou et al., and see the TNG-Cluster website at www.tng-project.org/cluster/. Reuploaded after acceptance for publication
The most massive galaxy clusters in the Universe host hundreds of massive satellite galaxies~$\mstar\sim10^{10-12.5} msun$, but it is unclear if these satellites are able to retain their own gaseous halos. We analyze the evolution of $\approx90,000$ satellites of stellar mass $\sim10^{9-12.5} msun$ around 352 galaxy clusters of mass $\mvir\sim10^{14.3-15.4} msun$ at $z=0$ from the new TNG-Cluster suite of cosmological magneto-hydrodynamical galaxy cluster simulations. The number of massive satellites per host increases with host mass, and the mass--richness relation broadly agrees with observations. A halo of mass $\mvirhost\sim10^{14.5} (10^{15}) msun$ hosts $\sim100 (300)$ satellites today. Only a minority of satellites retain some gas, hot or cold, and this fraction increases with stellar mass. Lower-mass satellites $\sim10^{9-10} msun$ are more likely to retain part of their cold interstellar medium, consistent with ram pressure preferentially removing hot extended gas first. At higher stellar masses $\sim10^{10.5-12.5} msun$, the fraction of gas-rich satellites increases to unity, and nearly all satellites retain a portion of their hot, spatially extended circumgalactic medium (CGM), despite the ejective activity of their supermassive black holes. According to TNG-Cluster, the CGM of these gaseous satellites can be seen in soft X-ray emission (0.5-2.0 keV) that is $\gtrsim10$~times brighter than the local background. This X-ray surface brightness excess around satellites extends to $\approx30-100$ kpc, and is strongest for galaxies with higher stellar masses and larger host-centric distances. Approximately $10$~percent of the soft X-ray emission in cluster outskirts $\approx0.75-1.5\rvir$ originates from satellites. The CGM of member galaxies reflects the dynamics of cluster-satellite interactions and contributes to the observationally inferred properties of the intracluster medium.
The morphology and kinematics of the gaseous circumgalactic medium of Milky Way mass galaxies -- II. comparison of IllustrisTNG and Illustris simulation results
The detectability of bars at high redshift: a case study using Euclid-like mock observations of TNG50 simulated galaxies
Universidade Tecnológica Federal do Paraná（巴西联邦技术大学巴拉那）；Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo（圣保罗大学天文、地球物理与大气科学研究所）；European Southern Observatory（欧洲南方天文台）；Aix Marseille Université, CNRS, CNES, LAM（艾克斯-马赛大学）；Universidade Federal do Rio de Janeiro, Observatório do Valongo（里约热内卢联邦大学瓦隆戈天文台）；Centro Brasileiro de Pesquisas Físicas（巴西物理研究中心）
Highly Ionized Oxygen in the Circumgalactic Medium of TNG100 Galaxies: Distributions, Thermal States, and Ionization Mechanisms
School of Physics and Astronomy, Tel Aviv University（特拉维夫大学物理与天文学学院）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）；Max-Planck-Institut für extraterrestrische Physik (MPE)（马克斯·普朗克地外物理学研究所）；Department of Physics, University of California, Berkeley（加州大学伯克利分校物理系）；Department of Astronomy, University of California, Berkeley（加州大学伯克利分校天文学系）
Inferring the mass of the circumgalactic medium using X-ray resonant scattering
University of Maryland, Baltimore County（马里兰大学巴尔的摩分校）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Universität Heidelberg（海德堡大学）；Stanford University（斯坦福大学）
Detectability of Satellite Planes in Mock Observations of Isolated L* Galaxies
Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）；Leibniz-Institut für Astrophysik Potsdam（波茨坦阿斯特罗物理莱布尼茨研究所）；Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院物理系天体物理实验室）；Clare Hall, University of Cambridge（剑桥大学克莱尔厅）
