标题： BASS LIII：爱丁顿比率是活动星系核中X射线辐射比例的主要调节者 显示英文标题

标题： BASS LIII: The Eddington Ratio as the Primary Regulator of the Fraction of X-ray Emission in Active Galactic Nuclei

摘要： 活动星系核（AGN）通过吸积在整个能量谱上发射辐射。 虽然标准的盘和冕模型可以部分描述这种辐射，但它无法预测诸如软X射线过量、短期光学/紫外变化以及AGN中观测到的紫外/X射线相关性等特定特征。 在此背景下，不同波段（即总辐射修正）中AGN辐射的比例有助于更好地理解AGN的吸积物理。 以往的研究表明，X射线总辐射修正强烈依赖于AGN的物理特性，如它们的光度和爱丁顿比率。 然而，由于这两个参数相互依赖，一直不清楚哪个是X射线总辐射修正的主要驱动因素。 我们在此呈现一项对硬X射线选择（14-195 keV）附近（$z<0.1$）AGN的大规模研究结果。 基于对236个无遮挡AGN的同时光学到X射线能谱分布的系统分析，我们发现控制X射线总辐射修正的主要参数是爱丁顿比率。 我们的结果表明，对于中间爱丁顿比率（$0.01-1$）的源，X射线总辐射修正随着总光度的增加而增加，但对于低爱丁顿比率（$<0.01$）的源，这种依赖关系消失。 这可能作为AGN在低爱丁顿比率下吸积物理发生变化的证据。 显示英文摘要

摘要： Active galactic nuclei (AGN) emit radiation via accretion across the entire energy spectrum. While the standard disk and corona model can somewhat describe this emission, it fails to predict specific features such as the soft X-ray excess, the short-term optical/UV variability, and the observed UV/X-ray correlation in AGN. In this context, the fraction of AGN emission in different bands (i.e., bolometric corrections) can be useful to better understand the accretion physics of AGN. Past studies have shown that the X-ray bolometric corrections are strongly dependent on the physical properties of AGN, such as their luminosities and Eddington ratios. However, since these two parameters depend on each other, it has been unclear which is the main driver of the X-ray bolometric corrections. We present here results from a large study of hard X-ray-selected (14-195 keV) nearby ($z<0.1$) AGN. Based on our systematic analysis of the simultaneous optical-to-X-ray spectral energy distributions of 236 unobscured AGN, we found that the primary parameter controlling the X-ray bolometric corrections is the Eddington ratio. Our results show that while the X-ray bolometric correction increases with the bolometric luminosity for sources with intermediate Eddington ratios ($0.01-1$), this dependence vanishes for sources with lower Eddington ratios ($<0.01$). This could be used as evidence for a change in the accretion physics of AGN at low Eddington ratios.