Speaker
Description
Shocks are key drivers of dust destruction in the interstellar medium (ISM), significantly influencing gas-phase element abundances. Feedback processes from active galactic nuclei (AGN), such as outflows and jets, generate shocks that create hostile environments where dust is expected to undergo extensive processing or destruction. However, recent observations reveal that dust grains and polycyclic aromatic hydrocarbons (PAHs)—essential tracers of star formation—can persist in such environments. The mechanisms underlying dust survival and processing in shocks remain poorly understood. In this talk, I will report on the detection of extended dust structures aligned with narrow-line regions (NLR) in a sample of nearby AGN using JWST/MIRI imaging. These dust features exhibit a striking morphological resemblance to the coronal gas emission ([Si VI]) and are aligned with AGN-driven outflows and the radio jet, regions where shocks are prevalent. Our analysis explores potential heating mechanisms for the dust, revealing that while AGN photoionization plays a significant role, it alone cannot account for the observed temperatures detected by JWST. These findings have significant implications for AGN feedback processes and the dust lifecycle, both of which are critical to our understanding of galaxy evolution.
