Jet Lamp-Post Models for Radio-Loud AGN

用于无线电大声 AGN 的射流灯柱模型

• 批准号: 467205901
• 负责人: Professor Dr. Jörn Wilms
• 金额: --
• 依托单位: Dr. Remeis-Sternwarte Bamberg - Astronomisches Institut -
• 依托单位国家: 德国
• 项目类别: Research Units
• 资助国家: 德国
• 项目状态: 未结题
• 来源: https://gepris.dfg.de/gepris/projekt/467205901?language=en
• 关键词: Jet; Lamp; Post; Models; Radio

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.

吸积黑洞的X射线观测通常揭示来自黑洞周围最内部区域的相对论反射特征（Dauser等人，2012; Duro等人，2016年; Jiang等人，这使我们能够测量它的自旋并探测X射线的主要来源“日冕”的位置。 对无线电安静物体的详细观察巩固了我们对黑洞附近致密日冕的看法。其性质仍有很大争议（帕克等人，2015; Beuchert等人，2017年）。一种可能的解释将其与亚发光喷流的基部和发射区域相联系（Markoff等人，2005; Dauser等人，2013; Wilkins等人，2017年）。虽然迄今为止分析的大多数来源都是塞弗特星系，但最近来自射电大声活动星系核（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年）。我们将用相对论喷流研究活动星系核中日冕的位置和性质。这是第一次，我们将分析一个样本的无线电响亮AGN与物理动机的相对论反射模型，由一个系统的倾斜，从VLBI测量的约束支持。 这种方法将使我们能够测量日冕的位置和大小，这将与P1的GRMHD模拟进行比较，以解决长期存在的问题，如果X射线日冕是相对论射流的基础。