AI 中文总结
该研究通过AESOPICA宇宙学模拟结合BALMERSOPICA模拟观测，解释了JWST早期AGN质量过大的现象，发现高效吸积可自然重现观测结果，为黑洞种子通道判别提供了方向。
AI 中文摘要
JWST在早期宇宙中发现的活动黑洞数量极多，且相对于本地标度关系显得质量过大，对标准的黑洞形成与增长模型提出了挑战。然而，目前仍不清楚这些黑洞是源于高效的早期增长通道、更广泛种群的可观测尾部，还是质量估计存在系统不确定性。我们推出AESOPICA项目，这是一套基于FABLE星系形成模型的12个中体积（$L=60\rm\thinspace Mpc$）宇宙学模拟，涵盖了理论形成通道中黑洞种子质量（$M_\rm{seed}=10^2$-$10^5\rm\thinspace M_\rm{\u2299}$）、包括超爱丁顿爆发在内的吸积效率以及超新星反馈强度的变化。我们通过BALMERSOPICA（一种模拟JWST宽线巡天的管道）对观测选择进行正向建模，该管道可针对给定光栅和曝光时间评估每个模拟活动星系核（AGN）的可探测性。我们发现，只要吸积效率足够高，JWST观测到的大部分AGN种群可由任意种子质量组装而成，尽管轻种子需要最有利的吸积条件。应用宽线选择会自然恢复看似质量过大的种群，对于吸积效率低的模型，探测到的AGN会偏离本征$M_\rm{BH}$-$M_\rm{stellar}$关系最远。值得注意的是，所选AGN位于本地、弱演化的$M_\rm{BH}$-$\rm{\u03C3}_\rm{stellar}$关系上，支持黑洞在恒星成分完全形成前就已组装的情景。由于高效吸积会快速消除初始种子质量的印记，黑洞质量函数的低质量端和宿主气体相金属丰度是区分种子形成通道最有前景的判别依据。
英文摘要
The active black holes uncovered by JWST in the early Universe are highly abundant and seemingly overmassive with respect to local scaling relations, challenging standard models of black hole formation and growth. Yet it remains unclear whether they trace an efficient early growth channel, the observable tail of a broader population, or suffer from systematic uncertainties in mass estimates. We introduce the AESOPICA project, a suite of twelve mid-volume ($L = 60\,\mathrm{Mpc}$) cosmological simulations based on the FABLE galaxy formation model, varying the black hole seed mass across the theoretical formation channels ($M_\mathrm{seed} = 10^{2}$-$10^{5} \, \mathrm{M_{\odot}}$), the accretion efficiency, including super-Eddington bursts, and the supernova feedback strength. We forward-model observational selection with BALMERSOPICA, a mock JWST broad-line survey pipeline that assesses the detectability of each simulated AGN for a given grating and exposure time. We find that the bulk of the JWST AGN population can be assembled from any seed mass provided the accretion efficiency is high, although light seeds require the most favourable accretion conditions explored. Applying broad-line selection naturally recovers the apparently overmassive population, with the detected AGN lying furthest above the intrinsic $M_\mathrm{BH}$-$M_\mathrm{stellar}$ relation for inefficient accretion models. Notably, the selected AGN lie on the local, weakly evolving $M_\mathrm{BH}$-$σ_\mathrm{stellar}$ relation, supporting a scenario where black holes assemble before the stellar component is fully established. Since efficient accretion rapidly erases the imprint of the initial seed mass, the low-mass end of the black hole mass function and host gas-phase metallicities offer the most promising discriminants between seeding channels.
Comments31 pages, 15 figures. Submitted to MNRAS. Comments welcome
