[Abridged] We present an analysis of the relation between the masses of cluster- and group-sized halos, extracted from $Λ$CDM cosmological N-body and hydrodynamic simulations, and their velocity dispersions, at different redshifts from $z=2$ to $z=0$. The main aim of this analysis is to understand how the implementation of baryonic physics in simulations affects such relation, i.e. to what extent the use of the velocity dispersion as a proxy for cluster mass determination is hampered by the imperfect knowledge of the baryonic physics. In our analysis we use several sets of simulations with different physics implemented. Velocity dispersions are determined using three different tracers, DM particles, subhalos, and galaxies.
We confirm that DM particles trace a relation that is fully consistent with the theoretical expectations based on the virial theorem and with previous results presented in the literature. On the other hand, subhalos and galaxies trace steeper relations, and with larger values of the normalization. Such relations imply that galaxies and subhalos have a $\sim10$ per cent velocity bias relative to the DM particles, which can be either positive or negative, depending on halo mass, redshift and physics implemented in the simulation.
We explain these differences as due to dynamical processes, namely dynamical friction and tidal disruption, acting on substructures and galaxies, but not on DM particles. These processes appear to be more or less effective, depending on the halo masses and the importance of baryon cooling, and may create a non-trivial dependence of the velocity bias and the $\soneD$--$\Mtwo$ relation on the tracer, the halo mass and its redshift.
These results are relevant in view of the application of velocity dispersion as a proxy for cluster masses in ongoing and future large redshift surveys.
The extended Baryon Oscillation Spectroscopic Survey: measuring the cross-correlation between the MgII flux transmission field and quasars and galaxies at $z=0.59$
Calibrating baryonic feedback with weak lensing and fast radio bursts
Ruhr University Bochum（鲁尔大学波鸿分校）；Argelander-Institut für Astronomie, Universität Bonn（波恩大学阿根兰德天文学研究所）；Ludwig-Maximilians Universität München（慕尼黑路德维希-马克西米利安大学）；Excellence Cluster ORIGINS（ORIGINS卓越集群）
Signatures of First Stars in Galaxy Surveys: Multi-Tracer Analysis of the Supersonic Relative Velocity Effect and the Constraints from the BOSS Power Spectrum Measurements
Backlighting the Cosmic Web with Fast Radio Bursts: An Anthology of Dispersion Measure Cross-Correlations with Large-Scale Structure and Baryon Tracers
California Institute of Technology（加州理工学院）；University of Arizona（亚利桑那大学）；University of Chicago（芝加哥大学）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）
Measuring the Angular Auto-power Spectrum of Fast Radio Burst Dispersion Measures as a Robust Cosmological Probe and Baryon Tracer
Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；School of Astronomy and Space Sciences, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）
Pinpointing the cosmic web between massive galaxy clusters I. The incidence of HI and OVI as WHIM tracers
Pontificia Universidad Católica de Valparaíso（智利天主教瓦帕莱索大学）；Universidad Técnica Federico Santa María（费德里科·圣塔玛丽亚理工大学）；Leibniz-Institut for Astrophysik Potsdam (AIP)（波茨坦阿基米德天体物理研究所）；The University of Tokyo（东京大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；New Mexico State University（新墨西哥州立大学）；University of Edinburgh（爱丁堡大学）；University of Washington（华盛顿大学）；CONICET-Universidad Nacional de Córdoba（阿根廷国家科学研究委员会-科尔多瓦国立大学）
Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution?
我们利用暗能量巡天（DES）第一年数据中发现的528个$0.2\leq z \leq 0.35$星系团的样本，探讨了团内漫射光（包括中央星系）和星系团（重子和暗）物质分布之间的关系。漫射光的表面亮度在较大的半径上表现出对团簇总质量的依赖性，并且在按团簇半径缩放后表现出具有普遍径向依赖性的自相似性。我们还比较了通过弱透镜测量的集群（重子和暗）物质分布的漫射光径向配置文件，并发现它们是可比的。IllustrisTNG星系形成模拟，TNG 300，提供了进一步的洞察扩散恒星质量和集群物质分布之间的联系-扩散恒星成分的模拟径向轮廓没有与总集群物质含量类似的斜率，虽然集群卫星星系的斜率。无论径向趋势如何，扩散恒星质量的数量与模拟中的星系团总质量具有低散射标度关系，优于星系团卫星星系的总恒星质量。我们的结论是，目前还没有一致的证据，是否漫射光是一个忠实的径向示踪剂的集群物质分布。然而，观测和模拟结果都表明，漫射光是星团总质量的一个很好的指标。
Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos
Case Western Reserve University（凯斯西储大学）；Universidad de Sevilla（塞维利亚大学）；Istituto Nazionale di Fisica Nucleare, Sezione di Bologna（意大利国家核物理研究所博洛尼分所）；Durham University（杜伦大学）；Harvard–Smithsonian Center for Astrophysics（哈佛-史密森天体物理中心）
A first measurement of baryonic feedback with Fast Radio Bursts
Argelander-Institut für Astronomie, Universität Bonn（波恩大学天体物理研究所）；Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians Universität München（慕尼黑大学物理学院天文台）；Excellence Cluster ORIGINS（ORIGINS卓越集群）
Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063
Baryonification III: An accurate analytical model for the dispersion measure probability density function of fast radio bursts
Argelander-Institut für Astronomie, Universität Bonn（波恩大学阿根德天文学研究所）；Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, The University of Manchester（曼彻斯特大学物理学与天文学系乔德雷尔银行天体物理学中心）；Institute for Particle Physics and Astrophysics, ETH Zurich（苏黎世联邦理工学院粒子物理与天体物理研究所）；Department of Astronomy and Oskar Klein Centre, AlbaNova, Stockholm University（斯德哥尔摩大学阿尔巴诺瓦天文学与奥斯卡·克莱因中心）；Department of Astrophysics, University of Zurich（苏黎世大学天体物理学系）；Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians Universität München（慕尼黑大学物理学院大学天文台）；Excellence Cluster ORIGINS（卓越集群ORIGINS）
