AI 中文总结
该研究利用模拟追踪宇宙正午到$z = 0.5$的黑洞，与多数研究不同追踪黑洞本身。发现中心黑洞沿特定关系演化，偏离该关系有不同演化通道，各类型黑洞在相关平面占据特征区域，揭示黑洞位置是其历史的化石记录。
AI 中文摘要
黑洞质量与恒星质量（$M_\mathrm{BH}-M_\star$）平面中系统的分布不仅编码了星系及其中心黑洞的整体增长，还包括塑造其演化的过程。利用ASTRID和TNG300宇宙学模拟，追踪从宇宙正午（$z = 2$）到$z = 0.5$的大质量黑洞。与以往多数研究不同，此次追踪黑洞本身而非其原宿主星系。发现中心黑洞沿相对紧密、几乎与红移无关的$M_\mathrm{BH}-M_\star$关系演化，偏离该关系则追踪不同演化通道。如高质量中心黑洞通过合并增长并通过AGN动力学反馈使宿主星系熄灭；潮汐剥离使卫星在几乎固定的$M_\mathrm{BH}$下转移到更低的$M_\star$，在贫气系统中产生弱吸积、超大质量中心黑洞；在ASTRID中，卫星吸积和低效动力学摩擦产生相对于新宿主质量不足的游荡黑洞。这些种群在$M_\mathrm{BH}-M_\star$和特定黑洞吸积率 - 特定恒星形成率平面中占据特征区域，表明黑洞在这些平面中的位置是其动力学、吸积和反馈历史的化石记录。
英文摘要
The distribution of systems in the black hole (BH) mass-stellar mass ($M_\mathrm{BH}-M_\star$) plane encodes both the integrated growth of galaxies and their central black holes, and the processes that shape their evolution. Using the ASTRID and TNG300 cosmological simulations, we track massive BHs from cosmic noon ($z=2$) to $z=0.5$. TNG300 repositions BHs to the centers of their host galaxies at every time step, while ASTRID instead advances them under the resolved gravitational forces plus a subgrid dynamical friction model, allowing BHs to wander off-center when orbital decay is inefficient. We follow the BHs rather than their original host galaxies, thereby capturing central BHs, BHs in satellites, and wandering BHs. We find that central BHs in both simulations evolve along a tight, nearly redshift-invariant $M_\mathrm{BH}-M_\star$ relation that is broadly consistent with local empirical constraints. Departures from this relation trace distinct evolutionary channels in which mergers play a key role. Major galaxy mergers drive BH-BH coalescence that dominates the growth of the most massive central BHs. These BHs subsequently quench their hosts through active galactic nucleus (AGN) kinetic feedback. Minor mergers tidally strip satellites to lower $M_\star$ at nearly fixed $M_\mathrm{BH}$, producing weakly accreting, overmassive central BHs in gas-poor systems. In ASTRID, satellite accretion and inefficient dynamical friction generate wandering BHs that are undermassive relative to their new hosts and experience minimal accretion or merger-driven growth. A BH's location in the $M_\mathrm{BH}-M_\star$ and specific BH accretion rate-specific star formation rate planes is therefore a fossil record of its dynamical, accretion, merger, and feedback history.
Comments17 pages, 11 figures. Published in ApJ
Journal refEmma Jane Weller et al 2026 ApJ 1008 70
