1. MASSIVE BLACK HOLES: formation & evolution Martin Rees Cambridge University

2. Themes of this symposium 1*. Radiation,,accretion jets, winds, etc --- phenomenology and models.

3. 3C31: Optical Radio

4. Themes of this symposium 1*. Radiation,,accretion jets, winds, etc --- phenomenology and models. 2*. Do ‘holes’ obey the Kerr metric (testing strong- field GR, etc)? * straightforward scaling laws between stellar-mass and supermassive holes

6. Themes of this symposium 1*. Radiation,,accretion jets, winds, etc --- phenomenology and models. 2*. Do ‘holes’ obey the Kerr metric (testing strong-field GR, etc)? 3.Population and demography of supermassive holes: how do they form and evolve? * straightforward scaling laws between stellar-mass and supermassive holes

7. Observational progress in demography and evolution of holes (I) Ubiquity of holes in galaxies

8. Massive black holes? Yes Yes but black hole mass scales with bulge mass not total mass Some at least Maybe Giant Ellipticals/S0sSpiralsDwarfsGlobular Clusters

9. black hole mass scales with bulge mass stellar velocity dispersion of the bulge Kormendy 2003 Is this really tighter?

10. Observational progress in demography and evolution of holes (I)Ubiquity of holes in galaxies (II)Feedback from hole to galaxy

11. New clues from deep Chandra observations of Perseus Fabian et al 03a,b

12. Observational progress in demography and evolution of holes (I) Ubiquity of holes in galaxies (II) Feedback from hole to galaxy (III) Objects discovered at z > 6.

14. A very early assembly epoch for QSOs A very early assembly epoch for QSOs The highest redshift quasar currently known SDSS 1148+3251 at z=6.4 has estimates of the SMBH mass M BH =2-6 x10 9 M sun (Willott et al 2003, Barth et al 2003) As massive as the largest SMBHs today, but when the Universe was <1 Gyr old!

15. THE HIGHEST-REDSHIFT QUASARS Becker et al. (2000)

16. Fluctuation generator Fluctuation amplifier (Graphics from Gary Hinshaw/WMAP team) Hot Dense Smooth Cool Rarefied Clumpy Brief History of the Universe

18. COOL BARYONS: need to COOL the smallest halos with deep enough potential wells to allow this First ‘action’ happens in the smallest halos with deep enough potential wells to allow this (at (at z~20-30) Hierarchical Galaxy Formation: small scales collapse first and merge later to form more massive systems courtesy of M. Kuhlen First ‘seed’ black holes?

22. PopIII stars remnants (Madau & Rees 2001, Volonteri, Haardt & Madau 2003) Viscous transport + supermassive star (e.g. Haehnelt & Rees 1993, Eisenstein & Loeb 1995, Bromm & Loeb 2003, Koushiappas et al. 2004) Efficient viscous angular momentum transport + efficient gas confinement First black holes in pregalactic halos z≈10-30 Simulations suggest that the first stars are massive M~100-600 M sun ( Abel et al., Bromm et al.) Metal free dying stars with M>260M sun leave remnant BHs with M seed ≥100M sun (Fryer, Woosley & Heger) Bar-unstable self-gravitating gas + large “quasistar” (Begelman, Volonteri & Rees 2006) Transport angular momentum on the dynamical timescale, process cascades Formation of a BH in the core of a low entropy quasistar ~ 10 4 -10 6 Msun The BH can swallow the quasistar M BH ~10 3 -10 6 M sun M BH ~100-600 M sun

24. seed. accreting gas dynamically interacting Supermassive holes grow from seed pregalactic BHs. These seeds are incorporated in larger and larger halos, accreting gas and dynamically interacting after mergers. HIGHEST PEAKS OF DENSITY FLUCTUATIONS All models for first BHs predict a biased formation: in the HIGHEST PEAKS OF DENSITY FLUCTUATIONS at z~20-30

25. Quasar host Dark matter Galaxies M h = 5 x 0 12 M  M h = 5  10 12 M  M * = 10 11 M  SFR = 235 M  /yr M BH = 10 8 M  Quasars end up in cD galaxies at centres of rich galaxy clusters today M h = 2 x 10 15 M  Descendant M h = 2  10 15 M 

27. Formation and evolution of supermassive binaries 1. Dynamical friction 2. Binary hardening due to stars or accretion of gas 3. Gravitational radiation t  a 4 t  a Do they merge?

28. LISA Will see mergers of 10 5 –10 7 Msol black holes 2011?

29. Lisa sensitivity to massive black hole binaries

30. Dependence of merger rate on mass of minihalos in which first holes form

31. DWARF GALAXIES/ MINIHALOS ELLIPTICAL GALAXIES mass V esc (km/s) 1000 100 10 10 9 10 13 V recoil (km/s) Gravitational rocket Gravitational rocket binary center of mass recoil during coalescence due to asymmetric emission of GW (e.g. Fitchett 1983, Favata et al 2004, Blanchet et al 2005, Baker et al 2006) v rec ≤ 250 km/s « v esc from today galaxies ≈ v esc from high-z ones GR SIMULATIONS

32. at z >10 more than 80% of merging MBHs can be kicked out of their halo (Volonteri & Rees 2006) the gravitational rocket effect is a threat at the highest redshifts, when host halos are small and have shallow potential wells Can the merger process start early enough to Allow build-up of supermassive holes? Can the merger process start early enough to Allow build-up of supermassive holes?

33. Build-up of holes by accretion (a ) Is there a continuous gas supply from host halo? (b) When supply is super-critical:, is ’excess’ radiation trapped and/or? accretion inefficient, allowing rapid growth in hole’s mass ? Or is there a radiation-driven outflow? (spin?).

34. NOTE; Classic argument of Soltan (1982), which compares total mass of holes with total radiative output, implies that most of the mass is gained via ‘efficient’ accretion. But most ot the ‘e-folds’ (eg first 10% of mass) could be gained rapidly via inefficient accretion from Yu & Tremaine 2002  SMBH =2.5-3.5x10 5 M  Mpc -3   ~0.2 @ z<5  qso(0) =2.1x10 5 [0.1(1-  )/  ]M  Mpc -3 Elvis, Risaliti & Zamorani 2002

35. Eddington accretion  =0.2 super-Eddington accretion

36. Are massive black holes rapidly spinning? (affects maximal accretion efficiency, minimum variability timescale, importance of Blandford-Znajek energy extraction, etc) Spin is modified by BH mergers and the coupling with the accretion disc Spin is modified by BH mergers and the coupling with the accretion disc mergers can spin BHs either up or down; alignment with the disc spins up

37. spin evolution by BH mergers only spin evolution by BH mergers AND accretion

38. 1. Mass of the BH seed PopIII stars remnants M BH ~100-600 M sun Gas collapse via Post-Newtonian instability M BH ~10 5 -10 6 M sun 2. BH mergers Positive contribution: build-up of high masses Negative contribution (gravitational rocket) 3. Accretion rate Eddington-limited (continuous or intermittent) Super-Eddington (Excess swallowed or expelled?)