AGN Feedback. Andrew King. Dept of Physics & Astronomy, University of Leicester Astronomical Institute, University of Amsterdam. Heidelberg, July 2014

Transcription

1 AGN Feedback Andrew King Dept of Physics & Astronomy, University of Leicester Astronomical Institute, University of Amsterdam Heidelberg, July 2014

2 galaxy knows about central SBH mass velocity dispersion galaxy bulge Kormendy & Ho, 2013

3 how? SBH mass is completely insignificant: 10 3 bulge, so its gravity affects only a region R inf = G parsec 8 = /10 8, 200 = /200 km s 1 - far smaller than bulge why does the galaxy notice the hole?

4 well... SBH releases accretion energy 0.1 BH c erg galaxy bulge binding energy 2 b erg galaxy notices hole through energy release: `feedback

5 SBH host connection SBH in every large galaxy (Soltan) but only a small fraction of galaxies are AGN SBH grow at Eddington rate in AGN c 2 Ṁ = L = L Edd = 4 Gc apple,apple= electron scattering opacity AGN should produce Eddington winds

6 Super-Eddington Accretion most photons eventually escape along cones near axis disc most mass expelled as wind on average photons give up all momentum to outflow after ~ 1 scattering Ṁv = L Edd c

7 Eddington winds momentum outflow rate speed Ṁ out v = L Edd c v = c ṁ 0.1c = ṀEdd where ṁ = Ṁout/ṀEdd 1 energy outflow rate 1 2 2Ṁoutv = 2. c2 Ṁ out = 2 L Edd ' 0.05L Edd (King & Pounds, 2003: cf later cosmological simulations)

8 PG (Pounds & Reeves, 2009) P Cygni profile of iron K- alpha: wind with v ' 0.1c `ultrafast outflow -- `UFO

9 outflow affects galaxy bulge SBH releases accretion energy 0.1 BH c erg galaxy bulge binding energy 2 b erg even though only a fraction ( /2) ' 0.05 of accretion energy is in mechanical form, this is more than enough energy to unbind the bulge how does the bulge survive?

10 wind shock wind must collide with bulge gas, and shock what happens? either (a) shocked gas cools: or (b) shocked gas does not cool: `momentum driven flow negligible thermal pressure - most energy lost `energy driven flow thermal pressure > ram pressure Compton cooling by quasar radiation field very effective out to cooling radius R C pc (cf Ciotti & Ostriker, 1997, 2001) initial expansion into bulge gas is driven by momentum only

11 swept-up ambient gas, mildly shocked wind shock outer shock driven into ambient gas SBH ambient gas Eddington wind, v 0.1c

12 motion of swept-up shell total mass (dark, stars, gas) inside radius R of unperturbed bulge is tot (R) = 2 2 R G but swept-up gas mass (R) = 2f g G 2 R forces on shell are gravity of mass within R, and wind ram pressure: since gas fraction f g is small, gravitating mass inside R is ' tot (R): equation of motion of shell is d dt [(R)Ṙ]+G(R)[ + tot(r)] R 2 =4 R 2 v 2 = Ṁoutv = L Edd c where is the black hole mass

13 using (R), tot (R) thisreducesto apple d dt (RṘ)+G R = where = f gapple G 2 4 integrate equation of motion by multiplying through by RṘ: then R 2 Ṙ 2 = 2GR 2 2 apple1 R2 + constant

14 using (R), tot (R) thisreducesto apple d dt (RṘ)+G R = where = f gapple G 2 4 integrate equation of motion by multiplying through by RṘ: then R 2 Ṙ 2 = 2GR 2 2 apple1 if <, no solution at large R (rhs < 0) R2 + constant Eddington thrust too small to lift swept-up shell

15 using (R), tot (R) thisreducesto apple d dt (RṘ)+G R = where = f gapple G 2 4 integrate equation of motion by multiplying through by RṘ: then R 2 Ṙ 2 = 2GR 2 2 apple1 if <, no solution at large R (rhs < 0) R2 + constant Eddington thrust too small to lift swept-up shell but if >, Ṙ 2! 2 2, and shell can be expelled completely

16 critical value = f gapple G 2 4 ' remarkably close to observed no free parameter (f g 0.1) relation despite effectively (King, 2003; 2005) SBH mass grows until Eddington thrust expels gas feeding it

17 shells confined to vicinity of BH until = R. R inf few G pc

18 transition to energy-driven flow once reached close to quasar shocked gas cooled by inverse Compton effect (momentum-driven flow) but once >, R can exceed R C : wind shock no longer cools wind shock is adiabatic: hot postshock gas does P dv work on surroundings bulge gas driven out at high speed v e = apple 2 2 c 3f g 1/3 ' /3 200 km s 1

19 Zubovas & King, 2012a once BH grows to >, shock passes cooling radius => large-scale energy-driven flow

20 Velocity / kms energy--driven outflows rapidly converge to apple 1/3 2 fc v e ' 2 c ' 925 2/ f (f c/f g ) 1/3 km s 1 g and persist even after central quasar turns off Time / yr high velocity outflow at large radius also for other potentials: Zubovas & King, 2012b Velocity / kms Radius / kpc

21 density contrast => energy-driven outflow shock may be Rayleigh-Taylor unstable two phase medium: gamma rays and molecular emission mixed large--scale high speed molecular outflows, e.g. rk 231: galaxy bulge should produce gamma-ray emission

22 outer shock runs ahead of contact discontinuity into ambient IS: velocity jump across it is a factor ( + 1)/( 1): fixes velocity as v out = +1 2 Ṙ ' /3 200 lfc f g 1/3 km s 1 and radius as R out = +1 2 R outflow rate of shocked interstellar gas is Ṁ out = d(r out) dt = ( + 1)f g 2 G Ṙ Ṁ out ' /3 200 l1/3 yr 1

23 AGN feedback: Herschel (molecular outflows) rk 231 OH Outflow terminal velocity (obs): ~1.100 km/s R out (model) rk 231 ~1.0 kpc outflow rate (d/dt): SFR: gas mass (from CO): ~1.200 /yr ~100 /yr 4.2 x 10 9 depletion time scale ( gas /): ~4 x 10 6 yr mechanical energy: ergs mechanical luminosity: 1% L IR

24 Eddington winds momentum outflow rate speed Ṁ out v = L Edd c v = c ṁ 0.1c = ṀEdd where ṁ = Ṁout/ṀEdd 1 energy outflow rate 1 2 2Ṁoutv = 2. c2 Ṁ out = 2 L Edd ' 0.05L Edd

25 aiolino et al., 2013 Fig. 12. Correlation between the kinetic power of the outflow and the AGN bolometric luminosity. Symbols and colour-coding as in Fig. 8. The grey line represents the theoretical expectation of models of AGN feedback, for which P K,OF = 5%L AGN.Thereddashedlinerepresents the linear fit to our data, excluding the upper limits. The error bar shown at the bottom-right of the plot corresponds to an average error of ±0.5 dex.

26 spirals: bulge outflow pressure => disc star formation expanding shocked bulge gas galaxy disc bulge outflow pressurizes central disc, and stimulates star formation bulge quenched, disc briefly fired up?

27 inhomogeneous IS? if IS is patchy, of two-temperature effects important, not obvious that wind shocks always cool could outflows be energy-driven at all radii? (Faucher-Giguere & Quataert, 2012, Bourne & Nayakshin 2013, 2014) if most of mass in dense blobs, these feel only drag of wind

28 inhomogeneous IS? if most of mass in dense blobs, these feel only drag of wind in simple cases this is dimensionally ~ ram pressure - maybe -sigma OK? but not obvious -- e.g. D Alembert s paradox -- no drag on smooth objects

29 inhomogeneous IS? calculation of drag => boundary layer; unstable, numerically difficult instabilities producing blobs also numerically difficult two-fluid effects on Compton cooling also difficult! but observational distinction is clear: momentum-driven = small-scale energy-driven = large-scale

30 evidence for localised behaviour? 1. super--solar QSO abundances same gas swept up, turned into stars, recycled => enrichment in very centre of galaxy 2. removal of D cusps: repeated small--scale (momentum-driven) outflow and fallback very effective (cf Pontzen & Governato 2012, who used SNe (less mass, less effective) 3. inner parts of most galaxy discs do not show enhanced star formation => no energy-driven outflow most of the time 4. metals produced by stellar evolution in galaxy eventually expelled to large radii by energy--driven outflow -- CG

31 SBH feedback: summary AGN have Eddington winds, Ṁv = L Edd /c,v 0.1c Compton cooling by AGN radiation field effective out to R C. 0.5 kpc resulting momentum-driven flow establishes relation once > shock passes R C and flow become energy-driven, with v 1000 km s 1 and Ṁ out few 1000 yr 1 (molecular) galaxy bulge becomes `red and dead, but can stimulate disc SF divides localised from global behaviour: super-solar abundances in AGN, removal of D cusps (local) metal pollution of CG (local to global) for more details see King & Pounds, ARAA, 2015