Unveiling the accretion geometry of Mrk 509 through broadband X-ray spectroscopy

Nearby AGN offer unique laboratories for testing feedback models that aim to explain the observed correlations between supermassive black holes (SMBHs) and their host galaxies. The nearby, X-ray bright Seyfert 1 galaxy Mrk 509 stands out in this context, as previous observations revealed the presence of a prominent FeKa emission line complex, including both a narrow, neutral and stable core component, and a broad and variable component. In addition blue- and red-shifted absorption lines have been reported, suggesting the presence of out/inflow material. Motivated by this, we obtained a ~100 ks observation of Mrk 509 with XRISM/Resolve. This triggered a series of (quasi-) simultaneous DDT observations with XMM-Newton and NuSTAR to provide strong constraints on the broadband continuum and new insights into the accretion and ejection processes at work in this AGN. We investigated the origin of the X-ray soft excess, to disentangle the contribution of the warm corona and of the relativistic reflection. Reflection from both the innermost accretion disc and colder material (outer disc, torus and/or BLR) is also invoked to describe the multicomponent FeKa emission line, that dominates the broadband spectrum. Two warm absorbers acting as total and partial coverer of the two comptonizing coronae provide a good description of the data, suggesting the presence of discrete inner BLR clouds along the line of sight that produce strong complex absorption in the soft X-ray spectrum.