1. Spins of supermassive black holes in quasars and galaxies Jian-Min Wang ( 王建民 ) Institute of High Energy Physics Chinese Academy of Sciences, Beijing Dec 1, 2009, ITP

2. SMBH properties Physical BHs: mass, spin and charge Astrophysical SMBHs Growth: accretion and mergers Spins: accretion manner, mergers Formation: high redshift Duty cycle: activity, coevolution Obscuration: unification scheme

3. Outline Introduction: quasars and AGNs Introduction: quasars and AGNs Spins Spins 1) Spins: measured from X-rays 1) Spins: measured from X-rays 2) Spins: measured from  -rays 2) Spins: measured from  -rays 3) spins: cosmological evolution 3) spins: cosmological evolution Dual AGNs: gravitation wave Dual AGNs: gravitation wave Conclusions Conclusions open questions open questions

4. AGNs and Quasars: Introduction Observations: spectra and classifications Morphology Theoretical model

5. Spectral classification

6. Obscured AGNs by IR observatiosn

7. NGC 1068

9. NGC 5548 (AGN) versus NGC 3277 (Normal)

10. Accretion disks: AGNs and Quasars

11. Coevolution of SMBH and galaxies

12. Quasar evolution

13. Measuring SMBH spins from X-rays

14. BH accretion disk Release of Gravitational energy Accretion rates hot corona ADAFs (advection- dominated accretion flows) Geometry of Accretion

15. Measurements of SMBH spins from X-rays Spectral shape Last stable orbit: radiative efficiency a * : specific angular momentum Spectral shape + last stable orbit→ a *

16. Reflection of X-rays from cold disk

17. Line profiles: affected by the Doppler shifts and gravity

18. Dependences of profiles on parameters (Fabian et al. 1989; Laor 1990) Model parameters: orientation θ emissivity   R -β spins: a *

19. a * =0.998, β=0.5 On orientation

20. On spins

21. On β

22. ASCA observation of MCG 6-30-15 (Tanaka, et al. 1995, Nature, 375, 659 )

23. XMM/Newton observations (Fabian et al. 2002, MNRAS, 335, L1)

24. Suzaku observations (Miniutti et al. 2007, PASJ, 59, S315)

25. 2 Spins of SMBHs from  -rays: in M87 (Wang et al. 2008, ApJ, 676, L109; Li, Y. et al. 2009, ApJ, 699, 513 ) M87: M BH =3.2 ×10 9 M ⊙ ; D=16Mpc M87

26. Conclusions: 1)  t ≤ 2 days; 2) Non-beaming effects

27. GLAST/Fermi observations (Abado et al. 2009, ApJ, 707, 55)  -rays escaping from the central region

28. 28

29. 3 Spins: cosmological evolution t galaxy t QSO

31. Wang et al. (2006;2008): duty cycle Soltan (1982); Chokshi & Turner (1992); Yu & Tremaine (2002); Marconi et al. (2004):  =0.1 Main growth of SMBH is driven by accretion Understanding trigger of SMBHs: spins

32. Spin evolution:  -equation (Wang, Hu et al. 2009, ApJ, 697, L141)

33. Properties and advantages: 1) only depends on observables 2) deep survey data for δ: up to redshift z 3) no need to compare with local BH mass density 4) Spin evolution

34. Bolometric luminosity function and density (Hopkins et al. 2007)

35. Mass function and BH density (Vestergaard et al. 2008; 2009)

36. Results Luminosity density SMBH density Vestergaard et al. (2009) Duty cycle Hopkins et al. (2007)

37. Cosmological evolution of SMBH spins King & Pringle (2007;2008): random accretion

38. Random accretion: spin-down

39. Evidence for random accretion Schmidt (1997), Pringle (1998) jet/disk is randomly-orientated torus is randomly-orientated disk+torus+galaxy have random orientation. Munoz Marin (2007)

40. Numerical simulations (Berti & Volonteri 2008) Pure mergersMerger+standard accretionMerger+random accretion What is driving the random accretion onto SMBH?

41. 4 Dual AGNs: gravitational wave (Wang et al. 2009, ApJ, 705, L76) SDSS: Sloan Digital Sky Survey 87 type 2 AGN sample Measurements: redshifts Properties? Double peaked [O III] profile: T. Heckman (1980; 1981) Whittle (1985)

42. Kepler Relation

43. Liu, Shen, Strauss et al. (2009, arXiv: 0908:2426)

44. Kepler relation Merritt & Ekers (2002)

45. Conclusions 1 ) fast spins: in MCG -6-30-15 and M87 1 ) fast spins: in MCG -6-30-15 and M87 2) strong evolution of SMBH spins: spin-down 2) strong evolution of SMBH spins: spin-down 3) merging galaxies: dual AGNs 3) merging galaxies: dual AGNs

46. Open questions X-rays: more detailed and high energy solution  -rays: more observations Spin evolution: co-evolution of SMBHs and galaxies Mergers: major and minor mergers.

47. Thanks for Attention