Modelling observable signatures of jet-ISM interaction: thermal emission and gas kinematics

Relativistic jets are believed to have a substantial impact on the gas dynamics and evolution of interstellar medium (ISM) their host galaxies. In this paper, we aim draw link between simulations observable signatures jet-ISM interactions by analyzing emission morphology kinematics resulting from jet-induced shocks in simulated disc spherical systems. We find that laterally expanding forward shock energy bubble sweeping through ISM causes large-scale outflows, creating shocked high-velocity dispersion entire nuclear regions ($\sim2$ kpcs) hosts. The jetted systems exhibit larger velocity widths (> 800 km/s), broader Position-Velocity maps distorted symmetry disc's projected velocities than without jet. also investigate above quantities at different inclination angles observer with respect galaxy. Jets inclined its found be confined for longer times, consequently couple more strongly gas. This results prominent widths, not only along jet's path, but perpendicular them. Strong interaction jet can distort morphology. However, after escape initial confinement, jet-disc coupling is weakened, thereby lowering widths.