发表机构
Max-Planck-Institut für Astrophysik; Astronomical Institute, Graduate School of Science, Tohoku University; Department of Applied Physics, Faculty of Engineering, Kanagawa University; Department of Astronomy, School of Science, University of Tokyo; Academia Sinica, Institute of Astronomy and Astrophysics; Heidelberger Institut für Theoretische Studien（马克斯·普朗克天体物理学研究所; 东北大学理学研究科天文学系; 神奈川大学工学部应用物理系; 东京大学理学部天文学系; 中央研究院天文及天文物理研究所; 海德堡理论研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过宇宙学辐射流体动力学模拟，发现富金属成簇恒星形成区可形成重种子黑洞与类小红点致密星团，揭示三者是强辐射弱富金属环境的关联产物。
AI 中文摘要
早期宇宙中超大质量黑洞（SMBH）的起源仍不确定。经典的直接坍缩场景要求原始气体暴露于强烈的莱曼-沃纳（LW）辐射中，但詹姆斯·韦布空间望远镜（JWST）的最新观测表明，早期成长中的黑洞可能位于致密的富金属环境中。我们利用宇宙学辐射流体动力学模拟研究早期黑洞的形成，该模拟自洽地追踪了快速吸积超大质量恒星（SMS）的形成与演化。我们发现，在成簇的恒星形成区中会产生强烈的LW辐射；到第一个重种子形成时，质量加权的内部强度已达到$J_{21}\backsim1000$。大多数种子形成于金属丰度为[Z/H]$\backsim-3$至$-2$的弱富金属气体中，因为最强的LW场出现在已被前期恒星反馈富集的区域。在我们的放大区域中，所有质量超过$10^9M_\u2609$的暗晕都拥有质量大于$10^5M_\u2609$的黑洞。我们使用MIST/PHOENIX恒星光谱库构建正常恒星的光谱，并用6000K黑体光谱构建膨胀SMS的光谱。在8个恒星质量大于$10^6M_\u2609$的大质量星团中，有5个表现出与类小红点（LRDs）相似的本征V形光谱。在最显著的案例中，发光的SMS主导了红色光学发射，尽管正常恒星族群的巴尔末跃变也有贡献。我们还在模拟中识别出中心偏离的类LRD系统，其与近期强引力透镜观测报道的系统相似。我们的结果表明，重种子形成、致密星团形成和类LRD连续谱发射是成簇、弱富金属、强辐射环境的关联产物。
英文摘要
The origin of supermassive black holes (SMBHs) in the early Universe remains uncertain. While the classical direct-collapse scenario requires pristine gas exposed to intense Lyman-Werner (LW) radiation, recent JWST observations suggest that early growing BHs may reside in compact, metal-enriched environments. We investigate early BH formation using a cosmological radiation-hydrodynamic simulation that self-consistently follows the formation and evolution of rapidly accreting supermassive stars (SMSs). We find that intense LW radiation develops in clustered star-forming regions; by the time the first heavy seed forms, the mass-weighted internal intensity has reached $J_{21}\sim1000$. Most seeds form in weakly metal-enriched gas with [Z/H]$\sim-3$ to $-2$, because the strongest LW fields occur in regions already enriched by previous stellar feedback. All halos above $10^9M_\odot$ in our zoom-in region host a BH more massive than $10^5M_\odot$. We construct stellar spectra using MIST/PHOENIX libraries for normal stars and $6000~\mathrm{K}$ blackbody spectra for bloated SMSs. Five of eight massive clusters with stellar masses larger than $10^6~M_\odot$ exhibit intrinsically V-shaped spectra similar to those of Little Red Dots (LRDs). In the most prominent cases, luminous SMSs dominate the red optical emission, although Balmer breaks in normal stellar populations also contribute. We also identify off-center LRD-like systems in our simulation resembling those recently reported in strongly lensed observations. Our results suggest that heavy-seed formation, compact-cluster formation, and LRD-like continuum emission are linked outcomes of clustered, weakly metal-enriched, strongly irradiated environments.
Comments19 pages, 13 figures
