Presentation #100.63 in the session AGN.
Outflows in active galactic nuclei (AGN) are considered promising candidates for driving AGN feedback on large scales. It is, however, notoriously challenging to access their kinetic power because of our limited knowledge of their density and spatial location. The key to obtaining this crucial information is to measure how the outflow responds to changes in the AGN continuum luminosity. Recently, I developed a new time-dependent photoionization (TPHO) model to characterize the time behaviour of the X-ray wind spectral features and determine the gas density (Rogantini et al. 2022). Specifically, TPHO allows precise mapping of the different outflows phases, providing a new important milestone in drawing the complete picture of the AGN structure. The exact estimate of the location and density of the ionized absorbers supplies the tightest constraints on the kinetic energy and the mass transferred to the surrounding medium. In this talk, I will present the results of the spectral-timing TPHO analysis of the new large XMM-Newton campaign of the variable AGN Mrk 355 taken in the summer of 2021. The source has not fully recovered yet the high flux shown before the obscuration event occurred in 2019 and its rich RGS spectra show the presence of multiple and variable fast ionized absorbers. I will describe the physics, structure, dynamics and energetics of these X-ray outflows focussing on their influence on the surrounding environment. Finally, I will present the power of the synergy between the TPHO model and the upcoming XRISM observations to determine the role of X-ray winds in AGN feedback.