Speaker: Dr. Dipanjan Mukherjee (University of Torino, Italy)
Relativistic jets from AGNs are an important driver of feedback in galaxies with an active black hole. They impact the nearby environment over different physical scales during their lifetime, with varying effects. They first interact with the host galaxy's ISM before breaking out to larger scales, significantly affecting the galaxy's morphology and evolution. I shall present the results of our recent 3D relativistic (magneto) hydrodynamic simulations, performed on scales of several kpc, of AGN jets interacting with the ambient ISM and CGM. The young relativistic jets initially couple strongly with the turbulent ISM, driving fast moving lateral outflows of dense gas. We have performed a suite of simulations of different jet powers, ISM conditions and morphologies. While AGN activity can potentially quench star formation by driving outflows or inducing turbulence, we find that they can also potentially enhance star formation (positive feedback) in localised patches. I will discuss the observational signatures of such jet-ISM interactions predicted by our simulations (optical+radio) which will help constrain the models from observed results.