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
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
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
AGNs and Quasars: Introduction Observations: spectra and classifications Morphology Theoretical model
Spectral classification
Obscured AGNs by IR observatiosn
NGC 1068
NGC 5548 (AGN) versus NGC 3277 (Normal)
Accretion disks: AGNs and Quasars
Coevolution of SMBH and galaxies
Quasar evolution
Measuring SMBH spins from X-rays
BH accretion disk Release of Gravitational energy Accretion rates hot corona ADAFs (advection- dominated accretion flows) Geometry of Accretion
Measurements of SMBH spins from X-rays Spectral shape Last stable orbit: radiative efficiency a * : specific angular momentum Spectral shape + last stable orbit→ a *
Reflection of X-rays from cold disk
Line profiles: affected by the Doppler shifts and gravity
Dependences of profiles on parameters (Fabian et al. 1989; Laor 1990) Model parameters: orientation θ emissivity R -β spins: a *
a * =0.998, β=0.5 On orientation
On spins
On β
ASCA observation of MCG (Tanaka, et al. 1995, Nature, 375, 659 )
XMM/Newton observations (Fabian et al. 2002, MNRAS, 335, L1)
Suzaku observations (Miniutti et al. 2007, PASJ, 59, S315)
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
Conclusions: 1) t ≤ 2 days; 2) Non-beaming effects
GLAST/Fermi observations (Abado et al. 2009, ApJ, 707, 55) -rays escaping from the central region
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3 Spins: cosmological evolution t galaxy t QSO
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
Spin evolution: -equation (Wang, Hu et al. 2009, ApJ, 697, L141)
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
Bolometric luminosity function and density (Hopkins et al. 2007)
Mass function and BH density (Vestergaard et al. 2008; 2009)
Results Luminosity density SMBH density Vestergaard et al. (2009) Duty cycle Hopkins et al. (2007)
Cosmological evolution of SMBH spins King & Pringle (2007;2008): random accretion
Random accretion: spin-down
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)
Numerical simulations (Berti & Volonteri 2008) Pure mergersMerger+standard accretionMerger+random accretion What is driving the random accretion onto SMBH?
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)
Kepler Relation
Liu, Shen, Strauss et al. (2009, arXiv: 0908:2426)
Kepler relation Merritt & Ekers (2002)
Conclusions 1 ) fast spins: in MCG and M87 1 ) fast spins: in MCG 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
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.
Thanks for Attention