Footprints in the Wind: Probing X-ray Outflows in NGC 7469 using Near-Infrared Emission Lines

TL;DR

This study uses near-infrared emission lines observed by JWST to analyze X-ray outflows in NGC 7469, providing insights into the velocity structure and ionization state of AGN winds despite current X-ray spatial resolution limitations.

Contribution

It introduces a novel method of probing X-ray outflows through near-infrared lines with JWST, offering a multi-phase view of AGN winds in NGC 7469.

Findings

High ionization X-ray gas has the largest mass and energy in outflows.

Feedback processes are less efficient than theoretical expectations.

Multi-phase outflow analysis reveals complex wind structure.

Abstract

AGN winds play an important role in the co-evolution 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] 3.03 um. 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] 10.51 um) and coronal (e.g. [Ne V] 14.32 um) emission lines to offer a comprehensive multi-phase 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.