Speaker
Description
A variety of results obtained in the recent years are suggesting that not only the presence of gas outflows is a signature of the impact of the energy released by the active SMBH, but also the physical conditions of the gas in the central (kpc-scales) regions of galaxies can be used to trace such impact.
These effects have been seen in gas observed around both high and low luminosity AGN.
In this talk I will summarise some of the results obtained for a range of phases of the gas, from hot gas traced by X-ray observations to warm and cold molecular gas. The results from ALMA/NOEMA and, more recently, JWST are expanded this field as we speak!
I will focus in particular on the impact of (young) radio jets: while expanding in the ISM they can create a cocoon of shocked gas which can explain e.g. the extreme line ratios seen in the cold molecular gas, shocked gas at the origin of LINERs spectra, outflows and extended X-ray emission in the direction perpendicular to the jets. These are all elements that can have a relevance for connecting the impact of the AGN to the properties of the ISM in the host galaxy.
If time allows, I will present the case of 3C84 (NGC1275) as an example of connecting and closing the feeding and feedback loop, while helping building a circumnuclear stellar disc.