We present $24$ cosmological dark matter (DM)-only zoom-in simulations of a Milky Way analog with initial conditions appropriate for scenarios where non-cold dark matter (NCDM) is a fraction of the total DM abundance (f-NCDM models) as the second installment of the COZMIC suite. We initialize our simulations using transfer functions, $T_{\mathrm{f-NCDM}}(k)\equiv\sqrt{P_{\mathrm{f-NCDM}}(k)/P_{\mathrm{CDM}}(k)}$ (where $P(k)$ is the linear matter power spectrum), with an initial suppression similar to thermal-relic warm dark matter (WDM) followed by a constant-amplitude plateau. We simulate suppression wavenumbers $[22.8,~ 32.1,~ 41.8,~ 52.0,~ 57.1,~ 95.3]~\mathrm{Mpc}^{-1}$, corresponding to thermal-relic WDM masses $m_{\mathrm{WDM}}\in [3,~ 4,~ 5,~ 6,~ 6.5,~ 10]~\mathrm{keV}$, and plateau amplitudes $δ\in [0.2,~ 0.4,~ 0.6,~ 0.8]$. We model the subhalo mass function in terms of the suppression wavenumber and $δ$. Integrating these models into a forward model of the MW satellite galaxy population yields new limits on f-NCDM scenarios, with suppression wavenumbers greater than $46$ and $ 40~\mathrm{Mpc}^{-1}$ for $δ=0.2$, $0.4$, respectively, at $95\%$ confidence. The current data do not constrain $δ>0.4$. We map these limits to scenarios where a fraction $f_{\mathrm{WDM}}$ of DM behaves as a thermal relic, which yields the following bounds on cosmologies with a mixture of WDM and CDM: $m_{\mathrm{WDM}}>3.6,~ 4.1,~ 4.6,~ 4.9,~ 5.4~\mathrm{keV}$ for $f_{\mathrm{WDM}}=0.5,~ 0.6,~ 0.7,~ 0.8,~ 0.9$, respectively, at $95\%$ confidence. The current data do not constrain WDM fractions $f_{\mathrm{WDM}}<0.5$. Our results affirm that low-mass halo abundances are sensitive to partial suppression in $P(k)$, indicating the possibility of using galactic substructure to reconstruct $P(k)$ on small scales.
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 Comparison of Galacticus and COZMIC WDM Subhalo Populations
University of Southern California（南加州大学）；The Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；UCLA Physics and Astronomy（加州大学洛杉矶分校物理与天文学）
Probing the Nature of Dark Matter Self-Interactions Through Observations of Massive Black Hole Mergers
Vanderbilt University（范德堡大学）；Fisk University（菲斯克大学）；Flatiron Institute（平顿研究所）；Princeton University（普林斯顿大学）；The Observatories of the Carnegie Institution for Science（卡内基科学促进会天文台）；California Institute of Technology（加州理工学院）
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）
Dynamic Zoom Simulations of structure formation beyond standard cosmology
Università di Bologna（博洛尼亚大学）；INAF, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）；INFN, Sezione di Bologna（意大利国家核物理研究所博洛尼亚分部）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学 Kavli宇宙粒子与宇宙学前沿研究所（WPI））；Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学 Kavli宇宙粒子与宇宙学前沿研究所数据驱动发现中心）
Intracluster Light as a Probe for Dark Matter: Exploring Self-interacting Dark Matter and Cold Dark Matter with C-EAGLE Sims
Korea Astronomy and Space Science Institute (KASI)（韩国天文学与空间科学研究所）；Quantum Universe Center, Korea Institute for Advanced Study（量子宇宙中心，韩国高等研究院）；School of Physics, The University of Sydney（悉尼大学物理学院）；ARC Centre of Excellence for Dark Matter Particle Physics（暗物质粒子物理卓越研究中心）；Departamento de Física Teórica, Facultad de Ciencias M-8, Universidad Autónoma de Madrid（马德里自治大学理学院M-8理论物理系）；Natural Science Research Institute (NSRI), University of Seoul（首尔大学自然科学研究所）；School of Physics, Korea Institute for Advanced Study（韩国高等研究院物理学院）；School of Physics and Astronomy, University of Nottingham（诺丁汉大学物理与天文学院）；Center for Advanced Computation, Korea Institute for Advanced Study（韩国高等研究院先进计算中心）；University of Science and Technology (UST)（科学技术院）
Probing Atomic Dark Matter with Stellar Streams in Milky Way-Mass Galaxies
Princeton University（普林斯顿大学）；University of Pennsylvania（宾夕法尼亚大学）；Flatiron Institute（平顿研究所）；University of California, San Diego（加州大学圣地亚哥分校）；University of Washington（华盛顿大学）；Massachusetts Institute of Technology（麻省理工学院）
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）
TNGC-SIDM I: Evolution of massive cluster mergers under the self-interacting dark matter paradigm
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Yonsei University（延世大学）；Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文中心）；Universität Heidelberg（海德堡大学）；University of California, Davis（加州大学戴维斯分校）；Alma Mater Studiorum Università di Bologna（博洛尼亚大学）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天文物理研究所博洛尼亚空间科学与天文观测台）；INFN-Sezione di Bologna（意大利国家核物理研究所博洛尼亚分部）；Massachusetts Institute of Technology（麻省理工学院）；Philipps Universität Marburg（马尔堡菲利普斯大学）
