Uncovering the relationship between ultra-fast outflows and the X-ray region in active galactic nuclei

Ultra-fast outflows (UFOs), with outflow velocities of ~0.1-0.5c, have been detected in the 7-10 keV band of ~40% of sampled active galactic nuclei (AGNs) over the past decade. These high column density, highly ionised winds are thought to be driven by the central X-ray source via a radiation pressure or magnetohydrodynamic driving mechanism, launched from within ~100 rg of the black hole. There is, however, not a clear understanding of how the X-ray region and UFO are related, a crucial component in understanding how this mode of AGN feedback operates to significantly alter the evolutionary course of the host galaxy. To probe this relationship, we examine a sample of 20 Type 1 AGNs that were reported as having significant (>95% confidence) UFO detections in the literature. Using XMM-Newton EPIC-pn data across the broad 0.3-10 keV X-ray band, we implement a physically motivated reflection model to describe the underlying continuum. This method reveals that 4 AGNs are inconsistent with exhibiting a UFO, and finds several high-significance correlations of wind ionisation and column density with accretion rate, X-ray luminosity, disc inclination, and reflection fraction. Wind velocity is found to be more difficult to characterise. We perform XRISM Resolve and ATHENA X-IFU simulations to showcase the vast improvements in UFO science that will be achieved with data collected from these future missions