Speaker
Description
Active galactic nuclei (AGN) drive multiphase outflows via both radiative and jet modes. While these outflows are extensively studied using traditional tracers—such as [O III] for ionized gas and H₂ or CO for molecular gas—and ultra-fast outflows (UFOs) are identified via extreme X-ray absorption, the intermediate-to-high ionization phase remains poorly understood. This regime (up to $\sim 300\text{ eV}$) is energetically more significant than the [O III]-traced component but less extreme than UFOs. Tracing it requires broad optical-to-infrared spectral coverage, as optical high-ionization coronal lines are intrinsically faint and rarely detected in jetted AGN.In this work, we search for coronal line outflows using [Fe VII] and [Fe X] lines across a sample of nearby jetted AGN. We detect strong coronal emission lines in 11 sources, revealing a morphology distinct from that of low-ionization lines. By combining spatially resolved optical data with high-resolution L- and C-band VLA radio observations, we find that while these highly ionized structures extend along the jet axis in a few sources, they remain compact in others. Additionally, using archival JWST data for two sources, we confirm the presence of highly ionized outflows via multiple infrared coronal emission lines.Finally, we compare the morphology of these high-ionization outflows against larger radio jet structures extending up to several hundred kiloparsecs. While low-ionization outflows tend to align closely with the jet axis and exhibit extended structures, highly ionized outflows are typically more confined to the nuclear regions and do not strictly follow the jet direction. This suggests that less powerful jets may more efficiently drive or enhance low-ionization outflows compared to their highly ionized counterparts.