活动星系核与超新星反馈的质量依赖相互作用对早型星系L_X-T关系的塑造
The mass-dependent interplay of active galacitc nuclei and supernova feedback in shaping the $L_{\rm X}$--$T$ relation of early-type galaxies
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中文总结 AI 辅助
本研究通过MACER3D框架的3D流体模拟，揭示早型星系L_X-T关系的调控机制随星系质量变化，AGN与SN反馈的耦合作用对塑造该关系有关键影响。
中文摘要 AI 辅助
观测到的早型星系热气体的X射线光度-温度（L_X-T）关系与纯引力加热的预测显著偏离，为超新星（SN）和活动星系核（AGN）反馈等非引力过程提供了关键约束。我们采用多尺度AGN调控宇宙生态系统求解器3D（MACER3D）框架，通过高分辨率3D流体动力学模拟研究该关系的物理起源，模拟对象包括矮椭球星系、大质量椭球星系和星系团中心星系。为对比分析，我们开展了受控模拟，仅包含AGN风与SN反馈，排除宇宙流入和环境效应。主导调控机制强烈依赖暗物质晕质量：在星系团中心星系的情况中，单独的AGN风或SN反馈均无法充分抑制气体密度和L_X，同时包含两者时，它们的非线性耦合会抑制X射线辐射，产生的（L_X, T）值低于观测关系；加入AGN喷流反馈可解决该偏差。在大质量椭球星系中，纳入AGN反馈后模型预测与观测L_X-T关系大致吻合，表明AGN反馈主导SN反馈。在低质量端，矮星系模型也遵循观测趋势，单独包含SN或AGN反馈的模型预测低L_X，同时包含两者时，AGN风驱动的SN富集气体向中间半径的输运会提升金属丰度和辐射冷却，进而增加L_X，这种耦合过程建立了类似喷泉的循环，气体在星系内被反复抬升和循环。
英文摘要
The observed X-ray luminosity--temperature ($L_{\rm X}$--$T$) relation of hot gas in early-type galaxies deviates significantly from the prediction of purely gravitational heating, providing a key constraint on non-gravitational processes such as supernova (SN) and active galactic nucleus (AGN) feedback. We investigate the physical origin of this relation using high-resolution 3D hydrodynamical simulations with the multiscale AGN-regulated cosmic ecosystem resolver in 3D (MACER3D) framework, which we applied to a dwarf elliptical, a massive elliptical, and a cluster-central galaxy. For comparison, we performed controlled simulations that included AGN winds and SN feedback in isolation, excluding cosmological inflow and environmental effects. The dominant regulation mechanism depends strongly on the halo mass. In the cluster-central case, neither AGN winds nor SN feedback alone can sufficiently suppress the gas density and $L_{\rm X}$. When both are included, their nonlinear coupling suppresses the X-ray emission, producing ($L_{\rm X}$, $T$) values below the observed relation; this discrepancy can be resolved by incorporating AGN jet feedback. In massive elliptical galaxies, the inclusion of AGN feedback brings the model predictions into broad agreement with the observed $L_{\rm X}$--$T$ relation, indicating that AGN feedback dominates SN feedback. At the low-mass end, dwarf galaxy models also follow the observed trend. In this regime, models with either SN or AGN feedback alone predict low $L_{\rm X}$. When both are included, AGN wind-driven transport of SN-enriched gas to intermediate radii enhances the metallicity and radiative cooling, thereby increasing $L_{\rm X}$. This coupled process establishes a fountain-like circulation, in which gas is repeatedly lifted and recycled within the galaxy.
