Speaker
Description
AGN-driven jets are frequently observed in galaxies, yet their interaction with the host's ISM remains poorly understood. In our studies (Meenakshi et al. 2022a,b), we use results from resolved simulations of jet-ISM interactions within the nuclear regions of host galaxies to investigate the extent of ionization, thermal shocked emission, and shocked gas kinematics. Our analysis indicates that the thermal energy injected by the jet can extensively shock-ionize the dense gas. Jets inclined toward the disc plane couple more strongly with the ISM and ionize a larger fraction of gas in the disc compared to vertical jets. The jets also clear out the central regions of the host galaxy, allowing radiation to propagate further. However, self-shielding by the outer layers of dense clumps blocks the AGN's ionizing radiation and prevents it from affecting the inner regions. The jet-induced, laterally expanding forward shock of the energy bubble sweeping through the ISM creates large-scale outflows, resulting in shocked emission and high-velocity dispersion throughout the nuclear region of the host. These jets impact not only their immediate surroundings but also disturb the kinematics in regions far from their axis. However, once the jets escape their initial confinement, the jet-ISM coupling weakens, and the gas in the system begins to settle and cool down in the presence of the host's gravitational potential, resulting in lower shocked emission and velocity widths.
