Hydrodynamic simulations of the disk of gas around supermassive black holes (HDGAS) -I; Molecular gas dynamics

ABSTRACT We present hydrodynamic simulations of the interstellar medium (ISM) within circumnuclear disc (CND) a typical active galactic nucleus (AGN)-dominated galaxy influenced by mechanical feedback from an AGN. The are coupled with CHIMES non-equilibrium chemistry network to treat radiative-cooling and AGN-heating. A focus is placed on central 100 pc scale where AGN outflows ISM constrained observational Seyfert-2 galaxies. AGN-feedback models implemented different wind-velocity mass-loading factors. post-process simulation snapshots radiative-transfer code obtain molecular emission lines. find that inclusion promotes formation CO in clumpy dense regions surrounding supermassive black holes (SMBHs). CO(1-0) intensity maps (<6 Myr) CND seem match well observations NGC 1068 best for model 5000 km s−1 high factor. attempt discern between competing explanations apparent counter-rotating gas through analysis kinematic line emission. suggest could explain alignment-stability position-angle across radii around SMBH momentum energy loading wind. It drives out alignment long period time. position–velocity diagrams broad agreement predicted Keplerian rotation-curve without AGN, but exhibit larger degree scatter, better observations.