Abstract Active galactic nuclei (AGN) winds play an important role in the coevolution of supermassive black holes and their host galaxies, yet their driving mechanisms and impact on star formation remain subjects of active investigation. Critically, the lack of X-ray integral field units currently limits our ability to acquire spatially resolved velocity information in the X-ray regime. However, instead, this can be achieved using the James Webb Space Telescope. As part of an ongoing investigation of the nuclear feedback processes in the nearby luminous AGN NGC 7469, we present an analysis of the kinematics of the X-ray emitting outflows using near-infrared footprint lines such as Mg viii λ 3.03 μ m. These high-ionization emission lines are associated with the same gas analyzed in the X-ray, and thus can be used to probe the footprint of the X-ray wind’s velocity structure and ionization state. Thanks to the wide wavelength range available with JWST we also use nebular (e.g., S iv λ 10.51 μ m) and coronal (e.g., Ne v λ 14.32 μ m) emission lines to offer a comprehensive multiphase view of the outflows. We present mass and kinetic energy outflow rates and find that while the feedback processes in NGC 7469 are not efficient by theoretical benchmarks, the most massive and energetic component is the high ionization X-ray gas.
Feuillet et al. (Wed,) studied this question.