We have implemented a simple model to identify the likely sites of the first stars and galaxies in the high-resolution simulations of the formation of galactic dark matter halos of the Aquarius Project. The first star in a galaxy like the Milky Way formed around redshift z=35; by z=10, the young galaxy contained up to 30000 dark matter haloes capable of forming stars by molecular hydrogen cooling. These minihaloes were strongly clustered and feedback may have severely limited the actual number of Population III stars that formed. By the present day, the remnants of the first stars would be strongly concentrated to the centre of the main halo. If a second generation of long-lived stars formed near the first (the first star relics), we would expect to find half of them within 30kpc/h of the galactic centre and a significant fraction in satellites where they may be singled out by their anomalous metallicity patterns. The first halo in which gas could cool by atomic hydrogen line radiation formed at z=25; by z=10, the number of such first galaxies had increased to ~300. Feedback might have decreased the number of first galaxies at the time they undergo significant star formation, but not the number that survive to the present because near neighbours merge. Half of all the "first galaxies" that form before z=10 merge with the main halo before z~3 and most lose a significant fraction of their mass. However, today there should still be more than 20 remnants orbiting within the central ~30kpc/h of the Milky Way. These satellites have circular velocities of a few kilometers per second or more, comparable to those of known Milky Way dwarfs. They are a promising hunting ground for the remnants of the earliest epoch of star formation.
Too Many, Too Few, or Just Right? The Predicted Number and Distribution of Milky Way Dwarf Galaxies
通过对观测到的SDSS矮星系群的完全性修正，我们预测了DES和LSST巡天中发现的银河系矮星系的空间分布和数量。我们应用最大规模的在过去，最早的形成，最早的坠落玩具模型，一组暗物质模拟银河系/M31晕对探索本地体积模拟（ELVIS）。观测到的银河系矮星系在LSST时代的空间分布将区分最早的陷落和矮星系如何填充暗物质subhalos的其他简化模型。包括所有的玩具模型和模拟，在90%的置信度下，我们预测在300 kpc内总共有37-114 L $\gtrsim 10^3$ L $_{\odot}$侏儒和131-782 L $\lesssim 10^3$ L $_{\odot}$侏儒。这些L $\gtrsim 10^3$ L $_{\odot}$矮星的数量比以前的预测要低得多，这主要是因为我们使用了更新的探测极限，并且每个天空区域发现的SDSS矮星的数量越来越少。对于25.8 mag的有效$r_{\rm limit}$，我们预测：DES的3-13 L $\gtrsim 10^3$ L $_{\odot}$和9-99 L $\lesssim 10^3$ L $_{\odot}$侏儒，LSST的18-53 L $\gtrsim 10^3$ L $_{\odot}$和53-307 L $\lesssim 10^3$ L $_{\odot}$侏儒。这些巨大的预测范围确保了未来十年的近场兴奋与这些…
Joint Constraints on Fuzzy and Warm Dark Matter from Satellite Populations of the Milky Way and Andromeda
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Sciences, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Science Center for Chinese Space Station Survey Telescope, National Astronomical Observatories, Chinese Academy of Science（中国科学院国家天文台中国空间站巡天望远镜科学中心）；School of Physics and Technology, Wuhan University（武汉大学物理科学与技术学院）
The DORCHA suite: nature, nurture, and the phase space distribution of the Milky Way's high redshift progenitors today
Facultad de Físicas, Multidisciplinary Unit for Energy Science, Universidad de Sevilla（塞维利亚大学物理学院能源科学多学科单元）；School of Physics, University of Melbourne（墨尔本大学物理学院）；ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)（ARC三维全天体物理学卓越中心（ASTRO 3D））；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）
Rise of the forsaken relics: connecting present-day stellar streams and phase-mixed galaxies to the Epoch of Reionization
University of Pennsylvania（宾夕法尼亚大学）；Yale University（耶鲁大学）；University of California, Davis（加州大学戴维斯分校）；Universität Zürich（苏黎世大学）；The Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；California Institute of Technology（加州理工学院）
Multimessenger Constraints on Supermassive Dark Stars and Their Black Hole Remnants
International Center for Quantum-field Measurement Systems for Studies of the Universe and Particles (QUP,WPI), High Energy Accelerator Research Organization (KEK)（宇宙与粒子量子场测量系统国际中心（QUP,WPI），高能加速器研究机构（KEK））；Institute of Particle and Nuclear Studies (IPNS), High Energy Accelerator Research Organization (KEK)（粒子与核研究研究所（IPNS），高能加速器研究机构（KEK））；Graduate University for Advanced Studies (SOKENDAI)（综合研究大学院大学（SOKENDAI））；Kavli Institute for the Physics and Mathematics of the Universe (WPI)（宇宙物理与数学卡弗里研究所（WPI））
