We present a detailed comparison between numerical cosmological hydrodynamic zoom simulations and semi-analytic models (SAMs) run within merger trees extracted from the simulations. The high-resolution simulations represent 48 individual halos with virial masses in the range 2.4*10^11M_sun < M_Halo < 3.3*10^13M_sun. They include radiative H & He cooling, photo-ionization, star formation and thermal SN feedback. We compare with different SAM versions including only this complement of physical processes, and also ones including supernova driven winds, metal cooling, and feedback from AGN. Our analysis is focused on the cosmic evolution of the baryon content in galaxies and its division into various components (stars, cold gas, and hot gas). Both the SAMs and simulations are compared with observational relations between halo mass and stellar mass, and between stellar mass and star formation rate, at low and high redshift. The simulations turn out to have much higher star formation efficiencies (by about a factor of ten) than the SAMs. Therefore the cold gas is consumed much more rapidly in the simulations and stars form much earlier. Also, simulations show a transition between stellar mass growth that is dominated by in situ formation of stars to growth that is predominantly through accretion of stars formed in external galaxies. In SAMs, stellar growth is always dominated by in situ star formation. In addition, SAMs overpredict the overall gas accretion rates relative to the simulations, and overestimate the fraction of "hot" relative to "cold" accretion. We discuss the reasons for these discrepancies, and identify several physical processes that are missing in our SAM. We also highlight physical processes that are neglected in the simulations studied here, but which appear to be crucial in order to understand the properties of real galaxies.
Introducing the THESAN-ZOOM project: radiation-hydrodynamic simulations of high-redshift galaxies with a multi-phase interstellar medium
York University（约克大学）；The University of Texas at Dallas（德克萨斯大学达拉斯分校）；University of Pennsylvania（宾夕法尼亚大学）；The University of Tokyo（东京大学）；Institute for Fundamental Physics of the Universe（宇宙基本物理研究所）；University of Edinburgh（爱丁堡大学）；Massachusetts Institute of Technology（麻省理工学院）；University of Cambridge（剑桥大学）；Max Planck Institute for Astrophysics（马克斯·普朗克天体物理研究所）
The THESAN-ZOOM project: Star-formation efficiencies in high-redshift galaxies
Massachusetts Institute of Technology（麻省理工学院）；York University（约克大学）；Leibniz-Institut für Astrophysik Potsdam（波茨坦阿纳尼天体物理研究所）；The University of Texas at Dallas（德克萨斯大学达拉斯分校）；University of Pennsylvania（宾夕法尼亚大学）；The University of Tokyo（东京大学）；Institute for Fundamental Physics of the Universe（基础物理宇宙研究所）；University of Edinburgh（爱丁堡大学）；Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森尼天体物理中心）；University of Cambridge（剑桥大学）
Evaluating the flexibility of the MillenniumTNG galaxy formation model with multi-zoom re-simulations
Columbia University（哥伦比亚大学）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；IKERBASQUE, Basque Foundation for Science（伊克尔巴斯基克科学基金会）；Max-Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Center for Computational Astrophysics, Flatiron Institute（计算天体物理学中心，富尔顿研究所）
INAF-Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians-Universität München（慕尼黑大学物理学院大学天文台）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；Department of Astronomy and Astrophysics, The University of Chicago（芝加哥大学天体物理学系）；IFPU - Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；ICSC - Italian Research Center on High Performance Computing, Big Data and Quantum Computing（意大利高性能计算、大数据和量子计算研究中心）；INFN, Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；Intel Technology India Private Ltd（英特尔技术印度私人有限公司）；Dipartimento di Fisica e Astronomia "Augusto Righi", Alma Mater Studiorum Università di Bologna（博洛尼亚大学奥古斯托·里吉物理与天文系）
