尘埃升华半径作为1型AGN中窄Fe K α线发射体的外包络
The dust sublimation radius as an outer envelope to the bulk of the narrow Fe Kalpha line emission in Type 1 AGN
摘要：
Fe K α发射线是活动星系核（AGN）X射线谱中最普遍的特征，但其窄核的起源仍然不确定。在这里，我们调查的Fe核心的发射区的大小和测量的尘埃环的大小之间的连接在13个本地1型活动星系核。观测到的Fe K发射半径（R_fe）由X射线光栅光谱中的光谱分辨线宽确定，尘埃升华半径（R_dust）由光学/近红外混响时间滞后或分辨近红外干涉数据测量。这种直接的比较表明，在一个对象的基础上，尘埃升华半径形成一个外部信封的大部分铁K排放。R_fe与活动星系核中的R_dust匹配得很好，具有目前最好的约束线宽。在相当一部分没有清晰窄线核的天体中，R_f近似于或小于光学宽线区的半径。这些事实对我们的样本的环面几何形状施加了重要的约束。扩展环面，其中荧光气体的立体角的峰值远远超过尘埃升华半径可以排除。我们还测试了R_fe的光度标度，发现爱丁顿比不是决定我们样品中谱线位置的主要驱动因素。我们详细讨论了潜在的警告，由于数据分析和仪器的限制，简单的线建模，不确定的黑洞质量，以及样本选择，表明这些都是不可能的偏见，我们的核心结果。Astro-H上的量热计将很快大大增加可以进行线测量的参数空间，克服许多这些限制。
英文摘要：
The Fe Kalpha emission line is the most ubiquitous feature in the X-ray spectra of active galactic nuclei (AGN), but the origin of its narrow core remains uncertain. Here, we investigate the connection between the sizes of the Fe core emission regions and the measured sizes of the dusty tori in 13 local Type 1 AGN. The observed Fe K emission radii (R_fe) are determined from spectrally resolved line widths in X-ray grating spectra, and the dust sublimation radii (R_dust) are measured either from optical/near-infrared reverberation time lags or from resolved near-infrared interferometric data. This direct comparison shows, on an object-by-object basis, that the dust sublimation radius forms an outer envelope to the bulk of the Fe K emission. R_fe matches R_dust well in the AGN with the best constrained line widths currently. In a significant fraction of objects without a clear narrow line core, R_fe is similar to, or smaller than the radius of the optical broad line region. These facts place important constraints on the torus geometries for our sample. Extended tori in which the solid angle of fluorescing gas peaks at well beyond the dust sublimation radius can be ruled out. We also test for luminosity scalings of R_fe, finding that Eddington ratio is not a prime driver in determining the line location in our sample. We discuss in detail potential caveats due to data analysis and instrumental limitations, simplistic line modeling, uncertain black hole masses, as well as sample selection, showing that none of these is likely to bias our core result. The calorimeter on board Astro-H will soon vastly increase the parameter space over which line measurements can be made, overcoming many of these limitations.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
