Overmassive black hole galaxies (OBGs) at redshifts $z \sim$ 10, or 450 Myr after the Big Bang, are one of the most puzzling discoveries by the James Webb Space Telescope to date because they formed by such early epochs and their black-hole to stellar mass ratios are a hundred times higher than those in galaxies today. Here we show that OBGs are simply the result of DCBH birth in primordial halos at early times. A 70,000 M$_{\odot}$ DCBH forming at $z =$ 25.7 in our cosmological simulation grows at about half the Eddington rate to $6.0 \times 10^6$ M$_{\odot}$ by $z =$ 10.1. Its host galaxy reaches a stellar mass of $4 \times 10^8$ M$_{\odot}$, a metallicity $Z =$ 0.1 Z$_{\odot}$, a star formation rate of 2 M$_{\odot}$ yr$^{-1}$, and $M_{\rm BH}/M_{\ast}$ $\sim$ 0.01, on par with OBGs like GN-z11, UHZ1, and GHZ9 at $z =$ 10.6, 10.1, and 10.2, respectively. Our simulation, the first to follow the coevolution of a DCBH and its host galaxy for several hundred Myr, shows that this ratio is a natural result of initial suppression of star formation by the DCBH and the later, violent blowout of metals by Pop III supernovae. Our models provide an excellent match to the spectra of UHZ1 and GHZ9 at $z =$ 10.1 and 10.4, respectively.
Episodic super-Eddington accretion as a clue to Overmassive Black Holes in the early Universe
Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Como Lake Center for Astrophysics, DiSAT, Università degli Studi dell’Insubria（因苏布里亚大学DiSAT科莫湖天体物理学中心）；INAF/Osservatorio Astronomico di Roma（罗马天文台（意大利国家天体物理研究所））；INFN, Sezione Roma1, Dipartimento di Fisica, “Sapienza” Università di Roma（罗马第一大学物理系意大利国家核物理研究院罗马一分部）；Dipartimento di Fisica, “Sapienza” Università di Roma（罗马第一大学物理系）；Sapienza School for Advanced Studies（罗马第一大学高等研究学院）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）
Chemical signatures from the first stars embedded in metal-poor gas in galaxies at cosmic dawn
Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；DTU Space, Technical University of Denmark（丹麦技术大学空间部）；Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze（佛罗伦萨大学物理与天文学系）；INAF/Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎综合理工学院、巴黎西岱大学、法国原子能和替代能源委员会、法国国家科学研究中心、天体物理学信息与方法实验室）；Centre national d’études spatiales (CNES)（法国国家空间研究中心）
Planet Formation at Cosmic Dawn: Planetesimals in H$_2$O-Rich Disks Around Low-Mass Stars
Institut fur Astro- und Teilchenphysik, Universitaat Innsbruck（因斯布鲁克大学天体与粒子物理研究所）；Research Institute of Physics, Southern Federal University（南联邦大学物理研究所）；Institute of Cosmology and Gravitation, Portsmouth University（朴茨茅斯宇宙学与引力研究所）；Physics Department, College of Science, United Arab Emirates University（阿拉伯联合酋长国大学理学院物理系）；National Institute of Technology, Kochi College（高知技术学院）；Department of Physics, Graduate School of Science, Kyoto University（京都大学理学研究科物理系）；Center for Astrophysics, Harvard and Smithsonian（哈佛史密森尼天体物理中心）
Extragalactic Planetary Nebulae (xPNe). Chemical evolution and assembly histories of nearby galaxies using Oxygen and Argon abundances. From the local universe to cosmic dawn
Reaching the Metallicity Floor at $z\sim 10$: Lensed Star Clusters at Cosmic Dawn and Cosmic Noon
ICC, University of Barcelona（巴塞罗那大学天体物理学与气候研究所）；ICREA（加泰罗尼亚高级研究院）；Dipartimento di Fisica e Astronomia “Augusto Righi”–Università di Bologna（博洛尼大学物理与天文系）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚空间天体物理与天文观测站）
Gravitational Waves from Cosmic Dawn: Tracing Cosmic Black Hole Binaries with ET, LGWA, and LISA
INAF/Osservatorio Astronomico di Roma（罗马天文台）；INFN, Sezione Roma1（罗马第一分部意大利国家核物理研究所）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Sapienza School for Advanced Studies（萨皮恩扎高等研究学院）
Black Hole Feedback, Galaxy Quenching and Outflows at Cosmic Dawn: Analysis of the SEEDZ Simulations
Maynooth University（梅努斯大学）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；University of Cambridge（剑桥大学）；Universität Heidelberg（海德堡大学）；Georgia Institute of Technology（佐治亚理工学院）；University College Cork（科克大学学院）；Cardiff University（卡迪夫大学）；University of Edinburgh（爱丁堡大学）
FLAMINGO: Tracing the co-evolution of hot gas and black holes in galaxy groups and clusters
Astrophysics Research Institute, Liverpool John Moores University（利物浦约翰摩尔斯大学天体物理研究所）；Institute for Computational Cosmology, Department of Physics, University of Durham（杜伦大学物理学院计算宇宙学研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Lorentz Institute for Theoretical Physics, Leiden University（莱顿大学洛伦兹理论物理研究所）
