The physical properties of AGN outflows and their impact on host galaxies from low to high redshift
* Abstract
Feedback from AGN is considered the main physical mechanism to quench star formation in galaxies, at least at the high mass end of the galaxy population. This feedback is believed to operate through powerful, massive outflows driven by the energy release operated by the AGN. However, while outflows are ubiquitous in AGN, their impact on host galaxies and physical properties are still poorly known. In particular, measurements of the outflow physical properties still rely on very rough assumptions which must be overcome when dealing with the wealth of information provided by the new integral field spectroscopic observations. I will present the results from several observational programs targeting AGN host galaxies from low to high redshift and aimed to understanding the physical properties of the outflows and their impact on the host galaxies, using integral field spectroscopy. I will also present evidence for galaxy scale ionised outflows in four Ultra Fast Outflows hosts, showing relativistic X-ray winds observed at the nuclear scale. The momentum rates of these ionised outflows are comparable to those measured for the UFOs at sub-pc scales, indicating momentum-driven wind propagation, and discuss the implications of these findings.