How do AGN jets shape the disc’s evolution and kinematics?

AGN-driven jets are not so uncommon in out universe. Observations show that they can strongly influence the evolution of their host galaxies, with many radio galaxies exhibiting highly turbulent, disturbed gas and velocity dispersions far greater than those in non-jetted systems. A central question of my research is: can we reproduce these signatures in simulations and connect them directly to observations?

I address this using high-resolution simulations of AGN jets interacting with multiphase, fractal gas discs. My work investigates how jet power and orientation shape the ionization structure, shock excitation, and gas kinematics of the host’s discs. We also attempted to connect with several of the well-studied observed systems.

Some animations from the work:

Time evolution of ionization extent in Sim. B (vertical jet) and D (inclined jet). See The extent of ionization in simulations of radio-loud AGNs impacting kpc gas discs, for details.

Animations from Modelling observable signatures of jet-ISM interaction: thermal emission and gas kinematics. Time evolution of [OIII] flux,[OIII] weighted mean velocity and W80 widths for Sim D (top) and E (bottom) at 20 degrees (left) and 90 degrees (right) image plane.