Reionisation in the early Universe is likely driven by dwarf galaxies. Using cosmological radiation-hydrodynamic simulations, we study star formation and the escape of Lyman continuum (LyC) photons from mini-haloes with $M_{\rm halo} \le 10^8\,M_\odot$. Our simulations include a new thermo-turbulent star formation model, non-equilibrium chemistry, and relevant stellar feedback processes (photoionisation by young massive stars, radiation pressure, and mechanical supernova explosions). We find that feedback reduces star formation very efficiently in mini-haloes, resulting in the stellar mass consistent with the slope and normalisation reported in Kimm \& Cen and the empirical stellar mass-to-halo mass relation derived in the local Universe. Because star formation is stochastic and dominated by a few gas clumps, the escape fraction in mini-haloes is generally determined by radiation feedback (heating due to photo-ionisation), rather than supernova explosions. We also find that the photon number-weighted mean escape fraction in mini-haloes is higher ($\sim20$-$40\%$) than that in atomic-cooling haloes, although the instantaneous fraction in individual haloes varies significantly. The escape fraction from Pop III stars is found to be significant ($\ge10\%$) only when the mass is greater than $\sim$100\,\msun. Based on simple analytic calculations, we show that LyC photons from mini-haloes are, despite their high escape fractions, of minor importance for reionisation due to inefficient star formation. We confirm previous claims that stars in atomic-cooling haloes with masses $10^8\,M_\odot\le M_{\rm halo} \le 10^{11}\,M_\odot$ are likely to be the most important source of reionisation.
A Portrait of the Cosmic Reionisation History in the Context of the Early Dark Energy Model
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Peking University（北京大学）；Swinburne University of Technology（斯威本科技大学）；University of Arizona（亚利桑那大学）
Lyman-alpha haloes in the aftermath of reionisation
Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦阿内斯实验室莱布尼茨研究所）；School of Earth & Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Department of General Systems Studies, Graduate School of Arts and Sciences, The University of Tokyo（东京大学大学院人文社会系研究科一般系统研究领域）；Institute of Science and Technology Austria (ISTA)（奥地利科学技术研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）
On the unique evolutionary mechanisms of massive quiescent galaxies in the epoch of reionisation
Swinburne University of Technology（斯威本科技大学）；JWST Australia Data Centre [JADC], Swinburne Advanced Manufacturing and Design Centre [AMDC]（JWST澳大利亚数据中心，斯威本先进制造与设计中心）
Interpreting ALMA Observations of the ISM During the Epoch of Reionisation
我们目前的宇宙学，辐射流体动力学模拟星系形成的时期，再电离的努力对建模的星际介质（ISM）和解释ALMA观测。模拟和没有恒星辐射进行了比较，在大（百万秒差距），中间（几十千秒差距），和小（子千秒差距）尺度。在大尺度上，星系周围的致密区域在紫外光子穿透空隙之前首先恢复;然而，大量的中性气体仍然存在于晕中。中性气体的空间分布是高度动态的，并且与年龄超过几百万年的恒星存在反相关。对于我们具体的反馈实现，大多数金属保持在晕的维里半径内，并且它们按质量成比例地分布在电离和中性介质上。对于我们质量最大的星系${\rm M_h}\sim10^{11}$ M $_{\odot}$，大部分的CII和OI质量与冷中性团块有关。NII更分散，并在较温暖的气体中产生，而OIII则在具有较高电离参数的较热气体中产生，由光加热和超新星产生。如果ISM中存在较小的高金属丰度气体，那么这些离子的发射可能会被ALMA观测到，而星系的低金属丰度可能会导致这些系统低于本地[CII]-SFR关系。尘埃的存在会导致UV/Ly $α$和[CII]发射之间的空间偏移，正如Maiolino等人最近的观测所表明的那样。[OIII]可能在空间上与这两个分量偏移，因为它来自密度-温度相空间的不同部分。
Co-evolution of baryons and dark matter halos of LYRA dwarf galaxies
Durham University（杜伦大学）；European Southern Observatory（欧洲南方天文台）；Stockholm University（斯德哥尔摩大学）；University of Hawaii（夏威夷大学）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）
