Jet Lamp-Post Models for Radio-Loud AGN

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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.