Charleston SC 18 October 2011; JPO. Momentum Driving in AGN and Galactic Feedback. Co-conspirators*: E. Choi L. Ciotti P. Johansson T. Naab G. Novak D. Proga S.Y.Sazonov R.A.Sunyaev. Cartoon of Co-Evolution of Elliptical and MBH/AGN.
18 October 2011; JPOMomentum Driving in AGN and Galactic Feedback
One of many recent papers on this topic….
Title: The clustering of narrow-line AGN in the local Universe
Authors: Cheng Li, Guinevere Kauffmann, Lan Wang, Simon D.M. White, Timothy M.
Heckman, Y.P. Jing
Comments: 14 pages, 11 figures, submitted to MNRAS
We have analyzed the clustering of ~ 90,000 narrow-line AGN drawn from the
Data Release 4 (DR4) of the SDSS. We compute the cross-correlation between AGN
and a reference sample of galaxies, and compare this to results for control
samples of inactive galaxies matched simultaneously in redshift,stellar
mass,concentration, velocity dispersion and the 4000A break strength. We also
compare near-neighbour counts around AGN and around the control galaxies. On
scales larger than a few Mpc, AGN have almost the same clustering amplitude as
the control sample. This demonstrates that AGN host galaxies and inactive
galaxies populate dark matter halos of similar mass.On scales between 100kpc
and 1Mpc,AGN are clustered more weakly than the control galaxies. We use mock
catalogues constructed from high-resolution N-body simulations to interpret
this anti-bias, showing that the observed effect is easily understood if AGN
are preferentially located at the centres of their dark matter halos. On scales
less than 70 kpc, AGN cluster marginally more strongly than the control sample,
but the effect is weak. When compared to the control sample, we find that only
one in a hundred AGN has an extra neighbour within a radius of 70 kpc. This
excess increases as a function of the accretion rate onto the black hole, but
it does not rise above the few percent level. Although interactions between
galaxies may be responsible for triggering nuclear activity in a minority of
nearby AGN, some other mechanism is required to explain the activity seen in
the majority of the objects in our sample.
BAL Dominates because coupling is most efficient
= 9/v102For standard mech
Ψ > 0 changes the game.
This omission is strange, given the enormous observed hard X-ray luminosities of accreting black holes !
Conclusion: most energy emitted in UV, but weighted by photon energy it is in the X-Ray region
Observational determination of the mean AGN emitted spectrum from individual objects and the X-Ray-background.
Most work presented at this conference has taken as GIVEN the inflow to the central black hole. Understanding this “outer boundary condition” is critical to understanding the feedback/AGN wind problem. In all of the work that I will be describing a the Bondi radius is resolved and no assumption of Bondi flow is needed. The hydro code itself decides how much matter flows towards the central black hole.
Compton Temp and Radiative Heating the inflow to the central black hole. Understanding this
= 2 107 K
Independent of Optical/UV absorption and of direction (for isotropic initial emission).
Elementary Thermodynamics: kTgas -> <h> ~ kTC
QSO luminosity in grouped bursts. the inflow to the central black hole. Understanding this
Thermal gas radiation the inflow to the central black hole. Understanding this
10 40 ≤LX,gas ≤ 1042
Green: Old stars
Black: Gas emission
Note: “quiet” level now computed by high resolution code. Not “sub-Bondi”.
Recycled gas from planetary nebulae.
Galactic wind into ambient medium driven by AGN bursts with peak value at 100 Msolar/yr.
Luminosity Distribution as Observed and stars.
“Cooling flow” model
red: BH (solid= Eddington; dotted=accretion lum., dashed = absorbed)
green: STARS (solid = LsnIa; dotted = LsnII; dashed = thermalization of stell. mass losses)
green: STARS (dot-dashed=optical starburst; long-dashed = UV starburst)
black: ISM (solid = X-ray, dotted = bolometric)
At late times the gas mass in the galaxy is less than the ejected and consumed mass
TOP: solid = total BH accreted mass; dotted = ISM mass in the galaxy
BOTTOM: same as above, but for rates; dashed: mass loss rate from the galaxy as a wind
Y.-F. Jiang, L. Ciotti & JPO (2009)
Computational domain bounded by inner and outer BC A giant SNR!
No Rotation Rotation A giant SNR!
Vel & Density
No X-ray Heating X-ray Heating A giant SNR!
Higher density at outer boundary (x 10)
Possibility of background X-ray heating
Bursting more irregular than in 1-D case, infalling shells fragment via R-T instability.
Heckman et al, 613,109 (2004)
Greene & Ho, 637,131 (2007)
Ho, 699,626 (2009)
Accreting fragment via R-T instability.
After the party
Two-D hydrodynamic simulation (Novak & JPO; 2009) cf Fabian (2009)
3-D treatment ( fragment via R-T instability.E.Choi, P. Johansson, T. Naab &JPO):
H&S + mass and momentum + radiation +B limit
Add Bondi Criterion
Add Radiation Feedback
Higher fluctuation rate and slower accretion
Lower accretion rate
R < 2GMBH/(c2+v2)??
Thermal Feedback Rate
Momentum Feedback Rate
Oscillation between low and high Eddington ratios