The Properties of Little Red Dot Galaxies in the ASTRID Simulation
Carnegie Mellon University（卡内基梅隆大学）；Harvard & Smithsonian（哈佛大学与史密森尼学会）；Michigan Institute for Data and AI in Society（密歇根数据与人工智能社会研究所）；Institute for Advanced Study（高等研究院）；University of California, Riverside（加州大学河滨分校）
Patrick LaChance, Rupert A. C. Croft, Tiziana Di Matteo, Yihao Zhou, Fabio Pacucci, Yueying Ni, Nianyi Chen, Simeon Bird
备注：
16 pages, 12 figures; Published in the Open Journal of Astrophysics
We present simulated counterparts of the ``Little Red Dot'' (LRD) galaxies observed with JWST, using the large cosmological hydrodynamic simulation, ASTRID. We create mock observations of the galaxies ($5 \leq z \leq 8$) in ASTRID, and find seventeen which fit the color and size criteria of LRDs. These LRDs are galaxies with high stellar masses ($\rm log(M_*/M_{\odot}) \geq 9.7$), and massive black holes ($\rm log(M_{BH}/M_{\odot}) \geq 6.8$). The host galaxies are dense, with stellar half mass radii ($\rm 325\,pc \leq r_{{\rm half},*} \leq 620\,pc$), and dust attenuation in the F444W band above 1.25. Their star formation has been recently quenched. They host relatively bright AGN that are dust-obscured and contribute significantly to the rest-frame optical red slope and have relatively low luminosity in the rest-frame ultraviolet, where the host galaxy's stars are more dominant. These LRDs are in an evolutionary phase of miniquenching that is the result of AGN feedback from their massive black holes. The LRDs in ASTRID are bright with F444W magnitudes of $23.5-25.5$. The less massive and fainter galaxies in ASTRID lack the dust concentration necessary to produce the red slope of an LRD, though this could be an effect of limited resolution. Most of the highest Eddington black holes are not LRDs due to insufficient dust attenuation from their host galaxies, which are also experiencing relatively high star formation rates. This results in their spectra being too flat, despite their highly accreting black holes.
Super-Eddington accretion in high-redshift quasar hosts: Black-hole driven outflows, galaxy quenching, and the nature of little red dots
INAF/Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；INFN, Sezione di Milano-Bicocca（意大利国家核物理研究所米兰比可卡分部）；INAF, Osservatorio Astronomico di Bologna（意大利国家天体物理研究所博洛尼亚天文台）
Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学 Kavli天文学与天体物理研究所）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）
Formation of the Little Red Dots from the Core-collapse of Self-interacting Dark Matter Halos
Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理系）；Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院科维理天体物理与空间研究研究所）；Department of Physics, Tsinghua University（清华大学物理系）
The Little Red Dots Are Direct Collapse Black Holes
Black Hole Initiative, Harvard University（哈佛大学黑洞倡议项目）；Scuola Normale Superiore（比萨高等师范学院）；Department of Physics and Astronomy, Colby College（科尔比学院物理与天文系）
Massive Black Holes Seeded by Dark Matter -- Implications for Little Red Dots and Gravitational Wave Signatures
John A. Paulson School of Engineering and Applied Sciences, Harvard University（哈佛大学约翰·A·保尔森工程与应用科学学院）；Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究所）；Theory Division, Fermilab（费米实验室理论部）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学卡弗里天文学与天体物理研究所）
Little Red Dots as self-gravitating discs accreting on supermassive stars: Spectral appearance and formation pathway of the progenitors to direct collapse black holes
Niels Bohr International Academy, The Niels Bohr Institute（尼尔斯·玻尔国际学院，尼尔斯·玻尔研究所）；Center of Gravity, Niels Bohr Institute（引力中心，尼尔斯·玻尔研究所）；Department of Astrophysics, University of Zurich（苏黎世大学天体物理学系）
Little Red Dot $-$ Host Galaxy $=$ Black Hole Star: A Gas-Enshrouded Heart at the Center of Every Little Red Dot
MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理与空间研究所）；Institute of Science and Technology Austria (ISTA)（奥地利科学与技术研究所）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Princeton University（普林斯顿大学）；University of Geneva（日内瓦大学）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）
Halo assembly bias in the early Universe: a clustering probe of the origin of the Little Red Dots
Peking University（北京大学）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院科维理天体物理与空间研究）
Primordial Black-Hole-Based Pathways to Little Red Dots
Johns Hopkins University（约翰斯·霍普金斯大学）；Università degli Studi di Padova（帕多瓦大学）；INFN, Sezione di Padova（意大利国家核物理研究所帕多瓦分部）；CERN（欧洲核子研究组织）；Space Telescope Science Institute（太空望远镜科学研究所）；Niels Bohr International Academy, Niels Bohr Institute（尼尔斯·玻尔国际学院，尼尔斯·玻尔研究所）
Van Swinderen Institute for Particle Physics and Gravity, University of Groningen（格罗宁根大学范斯温德恩粒子物理与引力研究所）；Department of Physics & Astronomy, University of the Western Cape（西开普大学物理与天文系）
Mass and Spin Growth of Very Massive Stars in Star Clusters Potentially Associated with Little Red Dots
Fukui Prefectural University（福井县立大学）；Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Yukawa Institute for Theoretical Physics, Kyoto University（京都大学汤川理论物理研究所）
NANOGrav 15-year gravitational-wave signals from binary supermassive black-holes seeded by primordial black holes, and implications for the origins of Little Red Dots
Graduate University for Advanced Studies (SOKENDAI)（高等研究院）；High Energy Accelerator Research Organization (KEK)（高能加速器研究机构）；National Astronomical Observatory of Japan（日本国立天文台）；University of Tokyo（东京大学）；The University of Tokyo（东京大学）
