In this paper, part of a series on the effects of X-ray sources in promoting Population III (Pop III) star formation, we investigate the ionisation and heating of the intergalactic medium (IGM) and the consequent enhancement of molecular hydrogen (H$_{2}$) and Pop III formation using cosmological zoom-in simulations. We adopt a minimal X-ray feedback model in which X-rays originate solely from Pop III supernovae, and compute the global X-ray and Lyman-Werner (LW) radiation backgrounds on-the-fly during the simulation of a mean-density region of the Universe. This approach self-consistently captures the feedback loop between Pop III stars and the radiation backgrounds they produce. Pop III supernovae generate a weak X-ray background (J$_{\mathrm{X,21}} \sim 10^{-5}$) and a moderate LW background (J$_{\mathrm{LW,21}} \sim 10^{-1}$); the latter intensifies below $z \approx 12$ (J$_{\mathrm{LW,21}} \sim 10^{1}-10^{2}$) with the onset of Pop II star formation. Applying these backgrounds to regions of varying mean density produces a net positive X-ray feedback that increases the Pop III number density, with stronger enhancement in underdense regions. The positive feedback is more pronounced when the X-ray background is computed on-the-fly rather than by post-processing, demonstrating the importance of the feedback loop. The X-ray background also raises the Thomson scattering optical depth at high redshift, while the total optical depth remains consistent with Planck 2018 constraints. Because our model includes only Pop III supernovae as X-ray sources, it represents the most conservative scenario; stronger X-ray feedback is expected when additional sources are included, as will be explored in future work.
Line Intensity Mapping Prediction from the Cosmic Dawn (CoDa) III Simulation for H$α$ from Galaxies and the Intergalactic Medium during the Epoch of Reionization
The Cosmic Ultraviolet Baryon Survey (CUBS) IX: The enriched circumgalactic and intergalactic medium around star-forming field dwarf galaxies traced by O VI absorption
本文基于 CUBS 数据通过 O VI 吸收线研究恒星形成矮星系周围的 CGM/IGM，发现低质量系统在 z≲1 时能有效将大量金属保留在附近的星系周与星系际介质中。
The Concerted Impact of Galaxies and QSOs on the Ionization and Thermal State of the Intergalactic Medium
我们使用一系列宇宙学、多频辐射转移（RT）模拟，详细分析了高红移类星体周围星系际介质（IGM）的电离和热结构，探索了星系和类星体的贡献，以及X射线和二次电离的影响。我们发现，在高z的类星体环境中的中央类星体和周围的星系协调控制的氢和氦的再电离形态，并对IGM的热结构的非线性影响。一个类星体的印记H II区域的一个独特的形态，如果它的总电离光子预算超过周围的星系，因为氢再电离的开始，否则，形态显示的H II区域只有星系产生的差异不大。此外，来自星系和类星体的集体辐射场的光谱形状控制着I-锋的厚度。虽然一个被紫外线遮蔽的类星体可以加宽I-锋，但来自其他紫外线源的贡献，无论是星系还是未被遮蔽的类星体，都足以维持一个尖锐的I-锋。来自类星体的X射线光子在I-锋之前造成了一个突出的部分电离延伸尾。类星体在He II / He III区的形态上留下了独特的印记。我们建议，虽然IGM的物理状态被修改的类星体，最直接的测试，以了解星系和类星体在再电离过程中的作用是进行星系调查，在天空中的21厘米层析成像的区域。
Quasar Radiative Feedback May Suppress Galaxy Growth on Intergalactic Scales at $z = 6.3$
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Augustana Campus, University of Alberta（阿尔伯塔大学奥古斯都校区）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理学与空间研究研究所）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理系）；Center for Frontier Science, Chiba University（千叶大学前沿科学中心）；Department of Physics, University of Oxford（牛津大学物理系）；Department of Astronomy, Tsinghua University（清华大学天文系）；Division of Particle and Astrophysical Science, Nagoya University（名古屋大学粒子与天体物理科学分部）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory - Astrophysics Group, University of Cambridge（剑桥大学卡文迪许实验室天体物理组）；Department of Physics and Astronomy, University College London（伦敦大学学院物理与天文系）；AURA for the European Space Agency (ESA), Space Telescope Science Institute（欧洲航天局（ESA）授权机构AURA，太空望远镜科学研究所）；Department of Astronomy, University of Michigan（密歇根大学天文系）
Discovery of Weak O VI Absorption in Underdense Regions of the Low-Redshift Intergalactic Medium
Space Telescope Science Institute（太空望远镜科学研究所）；Indian Institute of Technology Tirupati（印度理工学院蒂鲁帕蒂分校）；Indian Institute of Science Education and Research (IISER), Mohali（印度科学教育与研究学院（IISER），莫哈利）；Indian Institute of Space Science & Technology（印度空间科学与技术学院）；AURA for ESA, Space Telescope Science Institute（欧洲航天局AURA联盟，太空望远镜科学研究所）
Ultraviolet photon production rates of the first stars: Impact on the He II $λ$ 1640 Å emission line from primordial star clusters and the 21-cm signal from cosmic dawn
Uppsala University（乌普萨拉大学）；University of Cambridge（剑桥大学）；Indian Institute of Technology Indore（印度理工学院印多尔分校）
研究第一颗恒星的紫外光子产率及其对He II 1640 Å发射线和宇宙黎明时期21厘米信号的影响，探讨初始质量和旋转对光子产率的影响。
The impact of source and survey modelling on the connection between [O III] emitters and Ly $α$ forest transmission at z ~ 6
The University of Nottingham（诺丁汉大学）；University of Edinburgh（爱丁堡大学）；Kavli Institute for Cosmology（卡弗里宇宙学研究所）；Tata Institute of Fundamental Research（塔塔基础研究所）；Leibniz-Institut für Astrophysik Potsdam（波茨坦阿斯特拉物理研究所）
The formation of supermassive black holes from Population III.1 seeds. IV. Self-regulated seeding from supermassive star ionizing feedback
Chalmers University of Technology（查尔姆斯理工大学）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；University of Modena & Reggio Emilia（摩德纳与雷焦艾米利亚大学）；University of Oxford（牛津大学）；University of Memphis（孟菲斯大学）；Center for Astrophysics, Harvard and Smithsonian（哈佛史密松天体物理中心）；Università degli Studi di Trieste（的里雅斯特大学）；INAF - Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；INFN, Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）
