Jet Lamp-Post Models for Radio-Loud AGN

对吸合黑洞的x射线观测经常揭示黑洞周围最内层区域的相对论反射特征（Dauser et al., 2012; Duro et al., 2016; Jiang et al., 2018），这使我们能够测量其自旋并探测x射线的主要来源“日冕”的位置。对无线电安静天体的详细观测巩固了我们关于靠近黑洞的致密日冕的观点。其性质仍然存在强烈争议（Parker et al., 2015; Beuchert et al.,2017）。一种可能的解释将其与亚发光射流的基地和发射区域联系起来（Markoff等人，2005；Dauser等人，2013；Wilkins等人，2017）。虽然迄今为止分析的大多数来源都是塞弗特星系，但最近来自无线电活动星系核（AGN）的高质量数据也显示了相对论反射的证据（Lohfink等人，2017；Bhatta等人，2018）。我们将用相对论性喷流研究AGN中日冕的位置和性质。我们将首次使用物理驱动的相对论反射模型分析无线电响亮AGN样本，该模型由VLBI测量约束的系统倾角支持。这种方法将使我们能够测量日冕的位置和大小，并将其与P1的GRMHD模拟进行比较，以解决长期存在的问题，即x射线日冕是否是相对论性喷流的基础。

X-ray observations of accreting black holes routinely reveal relativistic reflection features from the innermost regions around the black hole (Dauser et al., 2012; Duro et al., 2016; Jiang et al., 2018) which allow us to measure its spin and to probe the location of the primary source of X-rays, the “corona”. Detailed observations of radio quiet objects have consolidated our view of a compact corona close to the black hole. Its nature is still strongly debated (Parker et al., 2015; Beuchert et al.,2017). One possible interpretation connects it to the base and launching region of a sub-luminous jet (Markoff et al., 2005; Dauser et al., 2013; Wilkins et al., 2017). While most sources analyzed to date have been Seyfert galaxies, recent high-quality data from radio-loud Active Galactic Nuclei (AGN) have also shown evidence for relativistic reflection (Lohfink et al., 2017; Bhatta et al., 2018). We will investigate the location and nature of the corona in AGN with relativistic jets. For the first time, we will analyze a sample of radio-loud AGN with a physically motivated relativistic reflection model, supported by a system inclination that is constrained from VLBI measurements. This approach will allow us to measure the location and size of the corona, which will be compared to GRMHD simulations from P1 to address the long-standing question if the X-ray corona is the base of the relativistic jet.