Speaker
Description
XRISM has provided an unprecedented view of the emission and absorption lines in the X-ray. Notably, early results showed significant complexity to the Fe-Kalpha line profile in AGN, with clear contributions from at least three emitting structures: an inner disc, intermediary broad line region (BLR), and an outer torus. This poses a new challenge for the modelling of the emission lines, which will only become more prominent with NewAthena. While fast sophisticated models exist for the disc line-profiles, large scale-height material is typically much more complex. In this talk I will present an analytic, yet physically motivated, approach for the emission line profiles from outflowing BLR scale material, motivated on reverberation and gravity+ studies which suggest at times an outflowing BLR. I will show that this gives a physically motivated, yet computationally fast, model for the intermediary component to Fe-Kalpha seen in the XRISM data, and demonstrate its application using the XRISM observations of NGC 4151. I will finish by discussing the future outlook, and how this approach can be extended for NewAthena to map not only the line profile but also its variability.