| Authors : | Moun Meenakshi, Dipanjan Mukherjee, Alexander Y. Wagner, Nicole P. H. Nesvadba,
Raffaella Morganti , Reinier M. J. Janssen, Geoffrey V. Bicknell, Ankush Mandal |
| Abstract : | The AGNs are known to affect the dynamics and evolution of their host's ISM. In our study, we aim to draw a link between the simulations and the observable signatures of several different aspects of AGN feedback on the central few kpcs of their host galaxy, namely shocked emission, shocked gas kinematics, and extent of ionization. We find that the jets produce large-scale outflows, and create high-velocity dispersion in the whole nuclear regions (~2 kpcs) of their host. Unlike galaxies without jets, the jetted systems exhibit larger velocity widths (>800 km/s), broader Position-Velocity maps, and disrupted symmetry in their projected velocity field. However, after the jets escape out from their host, the jet-disc coupling is weakened, resulting in decreased observable emission, and the reduced velocity dispersion in the central disc regions. We also show that the observable morphologies of kinematics and emission vary at different inclinations of the disc, and the observer sees different features of jet-ISM interaction at play. From the analysis of the extent of ionization, we find that the shocks from the jets (with kinetic power (10^{45} erg/s) can ionize a significant fraction (up to 33%) of dense gas (n > 100/cm^3) in the disc, and that the jets clear out the central regions of gas for AGN radiation to penetrate to larger distances in the disc. However, the radiation from an AGN of similar luminosity as the jet's power, is quickly absorbed by the outer layers of dense clouds in the disc, and is not able to substantially ionize the disc on a global scale. Thus, compared to jet-ISM interactions, we expect that photo-ionization by the AGN radiation only weakly affects the star-formation activity in the central regions of the galactic disc (>1 kpc), although the jet-induced shocks can spread farther out. |
