We investigate the distribution of metals in the cosmological volume at $z\sim3$, in particular, provided by massive population III (Pop III) stars using a cosmological $N$-body simulation in which a model of Pop III star formation is implemented. Owing to the simulation, we can choose minihaloes where Pop III star formation occurs at $z>10$ and obtain the spatial distribution of the metals at lower-redshifts. To evaluate the amount of heavy elements provided by Pop III stars, we consider metal yield of pair-instability or core-collapse supernovae (SNe) explosions of massive stars. By comparing our results to the Illustris-1 simulation, we find that heavy elements provided by Pop III stars often dominate those from galaxies in low density regions. The median value of the volume averaged metallicity is $Z\sim 10^{-4.5 - -2} Z_{\odot}$ at the regions. Spectroscopic observations with the next generation telescopes are expected to detect the metals imprinted on quasar spectra.
Intergalactic Medium Tomography with the Sunburst Arc
Texas Christian University（德克萨斯基督教大学）；University of Texas at Austin（得克萨斯大学奥斯汀分校）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；Kavli Institute for the Physics and Mathematics of the Universe (WIP)（宇宙物理与数学卡弗里研究所（WIP））；National Astronomical Observatory of Japan（日本国立天文台）；Stockholm University（斯德哥尔摩大学）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics（宇宙学物理卡弗里研究所）；University of Michigan（密歇根大学）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Auckland（奥克兰大学）；University of Cincinnati（辛辛那提大学）；University of Oslo（奥斯陆大学）；Goddard Space Flight Center（戈达德太空飞行中心）；Centre de Recherche Astrophysique de Lyon UMR5574（里昂天体物理研究中心）
Elevated Hot Gas and High-Mass X-ray Binary Emission in Low Metallicity Galaxies: Implications for Nebular Ionization and Intergalactic Medium Heating in the Early Universe
Exploring the influence of reionisation-era galaxies on their local intergalactic medium using the Sherwood-Relics simulations
Max Planck Institut für Astrophysik（马克斯·普朗克天体物理研究所）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；School of Physics and Astronomy, The University of Nottingham（诺丁汉大学物理与天文学院）；Department of Astronomy, University of Michigan（密歇根大学天文学系）；Leibniz-Institut für Astrophysik Potsdam（波茨坦莱布尼茨天体物理研究所）
Bubble mapping with the Square Kilometer Array -- I. Detecting galaxies with Euclid, JWST, WFIRST and ELT within ionized bubbles in the intergalactic medium at z>6
Two Populations of Carbon-Enhanced Metal-Poor Stars in the Disk System of the Milky Way
我们提出了一个低分辨率的化学动力学分析，AAOmega星系结构演化巡天（AEGIS）的恒星光谱（$R \sim 1300$），重点关注银河系盘系统内两个关键的碳增强贫金属（CEMP）恒星群：人口略有增加（$L_z < 1000\,$ kpc $\,$ km $\,$ s $^{-1}$）和强迁移（$L_z > 1000\,$ kpc $\,$ km $\,$ s $^{-1}$）群体。基于它们的化学和运动学特征，并与最近文献中发现的类似种群进行比较，我们初步将前者与源自$Gaia$香肠或$Gaia$ -土卫二的异位内晕种群联系起来。后一个种群与金属弱厚盘（MWTD）有关。我们讨论了它们的影响的背景下，银河系的形成历史。
