UniverseMachine：用放大模拟预测晕质量超过70年的星系恒星形成
UniverseMachine: Predicting Galaxy Star Formation over Seven Decades of Halo Mass with Zoom-in Simulations
摘要：
我们应用经验星系晕连接模型UniverseMachine的暗物质只放大模拟孤立的银河系（MW）的质量晕随着他们的父宇宙学模拟。这个应用程序扩展\textsc{UniverseMachine}预测到超微弱矮星系制度（$ 10^{2}\,\mathrm{M_{\odot}} \leqslant M_{\ast} \leqslant 10^{5}\,\mathrm{M_{\odot}}$），并产生一个良好的解决恒星质量晕质量（SMHM）的关系在峰值晕质量范围$10^8\,\mathrm{M_{\odot}}$ $10^{15}\,\mathrm{M_{\odot}}$。放大模拟提供的广泛的动态范围使我们能够评估\textsc{UniverseMachine}预测的矮星系演化的具体方面。特别是，虽然UniverseMachine不受约束的矮星系与$M_* \lesssim 10^{8}\,\mathrm{M_{\odot}}$，我们预测的SMHM关系是一致的推断MW卫星星系在$z=0$使用丰度匹配。然而，宇宙机器预测，几乎所有的星系都在$M_{\ast}\sim 10^{7}\,\mathrm{M_{\odot}}$以下活跃地形成恒星，这些系统通常在$z\lesssim 4$形成超过一半的恒星，这与有利于早期淬灭的本星系群矮星系的恒星形成历史不一致。这表明目前的宇宙机器模型并没有完全捕捉到低质量端的星系淬火物理。我们强调具体的改进，将环境和再电离驱动的淬火矮星系，并提供了一个新的工具，连接暗物质吸积恒星形成的整个动态范围内，主机星系。
英文摘要：
We apply the empirical galaxy--halo connection model UniverseMachine to dark matter-only zoom-in simulations of isolated Milky Way (MW)--mass halos along with their parent cosmological simulations. This application extends \textsc{UniverseMachine} predictions into the ultra-faint dwarf galaxy regime ($ 10^{2}\,\mathrm{M_{\odot}} \leqslant M_{\ast} \leqslant 10^{5}\,\mathrm{M_{\odot}}$) and yields a well-resolved stellar mass--halo mass (SMHM) relation over the peak halo mass range $10^8\,\mathrm{M_{\odot}}$ to $10^{15}\,\mathrm{M_{\odot}}$. The extensive dynamic range provided by the zoom-in simulations allows us to assess specific aspects of dwarf galaxy evolution predicted by \textsc{UniverseMachine}. In particular, although UniverseMachine is not constrained for dwarf galaxies with $M_* \lesssim 10^{8}\,\mathrm{M_{\odot}}$, our predicted SMHM relation is consistent with that inferred for MW satellite galaxies at $z=0$ using abundance matching. However, UniverseMachine predicts that nearly all galaxies are actively star forming below $M_{\ast}\sim 10^{7}\,\mathrm{M_{\odot}}$ and that these systems typically form more than half of their stars at $z\lesssim 4$, which is discrepant with the star formation histories of Local Group dwarf galaxies that favor early quenching. This indicates that the current UniverseMachine model does not fully capture galaxy quenching physics at the low-mass end. We highlight specific improvements necessary to incorporate environmental and reionization-driven quenching for dwarf galaxies, and provide a new tool to connect dark matter accretion to star formation over the full dynamic range that hosts galaxies.
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