We present results from the "Mint" resolution DC Justice League suite of Milky Way-like zoom-in cosmological simulations, which extend our study of nearby galaxies down into the ultra-faint dwarf regime for the first time. The mass resolution of these simulations is the highest ever published for cosmological Milky Way zoom-in simulations run to $z=0$, with initial star (dark matter) particle masses of 994 (17900) M$_\odot$, and a force resolution of 87 pc. We present initial results from these simulations, focusing on both satellite and near-field dwarf galaxies. We find that the simulated dwarfs and ultra-faint dwarfs (UFDs) reproduce the observed structural and dynamical properties of galaxies with $-3 < M_V < -19$. We predict the vast majority of nearby galaxies will be observable given the surface brightness limits of the Vera Rubin Observatory's co-added Legacy Survey of Space and Time (LSST). We additionally show that faint dwarfs with velocity dispersions $\lesssim5$ km/s result from severe tidal stripping of the host halo. These simulations allow us to investigate quenching of UFDs in a hydrodynamical Milky Way context for the first time. We find that the majority of the UFDs are quenched prior to interactions with the Milky Way, though some of the quenched UFDs retain their gas until infall. Additionally these simulations yield some unique dwarfs that are the first of their kind to be simulated, e.g., an HI-rich field UFD, a late-forming UFD that has structural properties similar to Crater 2, as well as a compact dwarf satellite that has no dark matter at $z=0$.

中文翻译：

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银河系环境中的超昏暗矮人：介绍薄荷条件 DC 正义联盟模拟

我们展示了来自“Mint”分辨率 DC 正义联盟套件的类似银河系的放大宇宙学模拟的结果，这首次将我们对附近星系的研究扩展到超微弱的矮星区域。这些模拟的质量分辨率是迄今为止公布的最高的宇宙银河系放大模拟运行至 $z=0$，初始恒星（暗物质）粒子质量为 994 (17900) M$_\odot$，以及力分辨率为 87 pc。我们展示了这些模拟的初步结果，重点是卫星和近场矮星系。我们发现模拟矮星和超微弱矮星 (UFD) 再现了观察到的星系的结构和动力学特性，$-3 < M_V < -19 $。鉴于维拉鲁宾天文台联合添加的时空遗产调查 (LSST) 的表面亮度限制，我们预测绝大多数附近的星系都可以观测到。我们还表明，具有速度色散 $\lesssim5$ km/s 的微弱矮星是由宿主晕的严重潮汐剥离造成的。这些模拟使我们能够首次在流体动力学银河系环境中研究 UFD 的猝灭。我们发现大多数 UFD 在与银河系相互作用之前就被淬灭，尽管一些淬灭的 UFD 会保留它们的气体直到坠落。此外，这些模拟产生了一些独特的矮星，它们是同类中第一个被模拟的，例如，富含 HI 的场 UFD，一种具有类似于火山口 2 的结构特性的晚期形成的 UFD，