Symphony: Cosmological Zoom-in Simulation Suites over Four Decades of Host Halo Mass
Ethan O. Nadler, Philip Mansfield, Yunchong Wang, Xiaolong Du, Susmita Adhikari, Arka Banerjee, Andrew Benson, Elise Darragh-Ford, Yao-Yuan Mao, Sebastian Wagne… 展开作者
Ethan O. Nadler, Philip Mansfield, Yunchong Wang, Xiaolong Du, Susmita Adhikari, Arka Banerjee, Andrew Benson, Elise Darragh-Ford, Yao-Yuan Mao, Sebastian Wagner-Carena, Risa H. Wechsler, Hao-Yi Wu
备注：
39 pages, 20 figures, 2 tables. Updated to published version
We present Symphony, a compilation of $262$ cosmological, cold-dark-matter-only zoom-in simulations spanning four decades of host halo mass, from $10^{11}$$-$$10^{15}~M_{\mathrm{\odot}}$. This compilation includes three existing simulation suites at the cluster and Milky Way$-$mass scales, and two new suites: $39$ Large Magellanic Cloud-mass ($10^{11}~M_{\mathrm{\odot}}$) and $49$ strong-lens-analog ($10^{13}~M_{\mathrm{\odot}}$) group-mass hosts. Across the entire host halo mass range, the highest-resolution regions in these simulations are resolved with a dark matter particle mass of $\approx 3\times 10^{-7}$ times the host virial mass and a Plummer-equivalent gravitational softening length of $\approx 9\times 10^{-4}$ times the host virial radius, on average. We measure correlations between subhalo abundance and host concentration, formation time, and maximum subhalo mass, all of which peak at the Milky Way host halo mass scale. Subhalo abundances are $\approx 50\%$ higher in clusters than in lower-mass hosts at fixed sub-to-host halo mass ratios. Subhalo radial distributions are approximately self-similar as a function of host mass and are less concentrated than hosts' underlying dark matter distributions. We compare our results to the semianalytic model $\mathrm{\texttt{Galacticus}}$, which predicts subhalo mass functions with a higher normalization at the low-mass end and radial distributions that are slightly more concentrated than Symphony. We use $\mathrm{\texttt{UniverseMachine}}$ to model halo and subhalo star formation histories in Symphony, and we demonstrate that these predictions resolve the formation histories of the halos that host nearly all currently observable satellite galaxies in the universe. To promote open use of Symphony, data products are publicly available at http://web.stanford.edu/group/gfc/symphony.
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）
Symfind: Addressing the Fragility of Subhalo Finders and Revealing the Durability of Subhalos
SLAC National Accelerator Laboratory（SLAC国家加速器实验室）；Department of Physics, Stanford University（斯坦福大学物理系）；Carnegie Observatories（卡内基观测站）；Department of Astronomy, University of Maryland, College Park（马里兰大学帕克分校天文学系）
COZMIC. I. Cosmological Zoom-in Simulations with Initial Conditions Beyond Cold Dark Matter
University of California, San Diego（加州大学圣地亚哥分校）；Carnegie Observatories（卡内基观测站）；University of Southern California（南加州大学）；University of California, Los Angeles（加州大学洛杉矶分校）
A Unified Halo Mass Function Across Dark Matter Models from High-Resolution Multi-Scale Simulations
Carnegie Institution for Science（卡内基科学机构）；University of California, San Diego（加利福尼亚大学圣地亚哥分校）；University of California, Los Angeles（加利福尼亚大学洛杉矶分校）；University of Southern California（南加州大学）；Institute for Advanced Study（高等研究院）；Flatiron Institute（平顿研究所）
Predicting the Subhalo Mass Functions in Simulations from Galaxy Images
University of Montreal（蒙特利尔大学）；MILA Quebec AI Institute（MILA魁北克人工智能研究所）；Northwestern University（西北大学）；The NSF-Simons AI Institute for the Sky（NSF-西蒙斯天空人工智能研究所）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理中心）；Perimeter Institute for Theoretical Physics（理论物理珀米特研究所）；Trottier Space Institute, McGill University（麦吉尔大学特罗蒂尔空间研究所）；Kavli Institute for Cosmology（卡弗里宇宙学研究所）；Institute of Astronomy（天文研究所）；Princeton University（普林斯顿大学）
Efficiently emulating distribution functions in gigaparsec volumes for varying cosmological parameters
Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Department of Astronomy, Columbia University（哥伦比亚大学天文系）；Astronomy Centre, University of Sussex（萨塞克斯大学天文学中心）；Department of Physics, University of Connecticut（康涅狄格大学物理系）；Columbia Astrophysics Laboratory, Columbia University（哥伦比亚大学哥伦比亚天体物理学实验室）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）；Department of Physics and Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学物理与天文学系）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理科学系）
Solving Milky Way-sized Systems with Haskap Pie: A Halo finding Algorithm with efficient Sampling, K-means clustering, tree-Assembly, Particle tracking, Python modules, Inter-code applicability, and Energy solving
University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；National Center for Supercomputing Applications（超级计算应用国家中心）
The DREAMS Project: Disentangling the Impact of Halo-to-Halo Variance and Baryonic Feedback on Milky Way Dark Matter Speed Distributions
Princeton University（普林斯顿大学）；Flatiron Institute（西蒙斯平铺研究所）；University of Virginia（弗吉尼亚大学）；The NSF-Simons AI Institute for Cosmic Origins（NSF-Simons宇宙起源人工智能研究所）；Stockholm University（斯德哥尔摩大学）；University of Chicago（芝加哥大学）；University of Pennsylvania（宾夕法尼亚大学）；Massachusetts Institute of Technology（麻省理工学院）；Rutgers, the State University of New Jersey（新泽西州立罗格斯大学）；University of Texas at Austin（得克萨斯大学奥斯汀分校）
LYRA ultra-faints: The emergence of faint dwarf galaxies in the presence of an early Lyman-Werner background
Durham University（杜伦大学）；Stockholm University（斯德哥尔摩大学）；University of Hawaii（夏威夷大学）；University of Vienna（维也纳大学）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）
Abundance matching with the mean star formation rate: there is no missing satellites problem in the Milky Way above $\mathbf{M_{200} \sim 10^9\,{\rm \bf M}_\odot}$
