Cosmic Feedback from AGN

42 Pages·2011·3.73 MB·English

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