AC Fabian, M. Cappi, J Sanders Cosmic Feedback from AGN AC Fabian, M Cappi, J Sanders, S Heinz, E Churazov, B McNamara, J Croston, D Worrall, F Humphrey, F Tombesi, J Reeves, M Giustini, P O’Brien, T Reiprich P Nulsen, T Ponman, N Werner, W Forman, A Young, N Brandt, G Chartas Possible effect of central black hole on host galaxy E  30  E BlackHol e Gal axy Energy released by Gravitational growth of Black Binding Energy of Hole Host Galaxy 2 major modes for the interaction: Kinetic (radio/jet) and Radiative (quasar) KEY QUESTIONS 1) Understanding the energy flow in cool cor es of clusters, groups and ellipticals: ( …) Velocity field, bulk motions, shocks, turbulence 2) Understanding the energy and mass flow of AGN outflows: ( Mass and energy components, velocity structure, …) variability, ionization structure X-rays are most direct probe of crucial volume-filling component Cool Cores in Clusters X-ray brightest region in Clusters and Groups, with size ~100 kpc Radius of XMS FOV ~ 130 kpc at z~0.1, which is well matched to cool cores Need to map flows (velocities and line widths), Line strengths, metallicities etc Athena XMS offers order of magnitude (or more) improvement over ASTRO-H on spatial resolution and counts, and 2 on spectral resolution. Chandra 1.4 Ms M84 Hydra A Perseus Athena XMS simulation FoV • ~14 000 counts per pixel in brightest region in 50ks observation • Most of the structures are resolved with 10” PSF and much better than XMM • 5” PSF is desirable, but not required