Speaker
Description
Active galactic nuclei (AGNs) influence their host galaxies through powerful winds that drive large-scale outflows, regulating star formation by heating, removing, or compressing the interstellar medium (ISM). Despite their importance for galaxy–supermassive black hole co-evolution, the impact of AGN-driven feedback on the surrounding molecular gas reservoir remains poorly understood. In this talk, we present a first kinematics study of outflowing molecular gas in a typical circumnuclear disk (CND) using a 3D radiative transfer code coupled with kinematic models. We explore both a fully outflowing disk and a partially outflowing disk in which the outflow velocity depends inversely on gas density. For the fully outflowing CND, we find that increasing outflow velocity, increasing outflow inclination, and decreasing disk compactness all lead to more complex synthetic line profiles, with additional strong effects on the line-of-sight velocity centroids and component widths. In the partially outflowing case, the line profile structure similarly depends on the density–velocity relation. This work represents a first step toward a kinematics-based radiative transfer framework for extra-galactic circumnuclear environments, with future works including inner AGN structures such as the torus and combining radiative transfer with chemical modeling.
| Talk category | NOVA Network 1 |
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