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Masayuki UMEMURA Center for Computational Physics, University of Tsukuba, Japan

A Coevolution Scheme for Supermassive Black Holes and Galactic Bulges. Masayuki UMEMURA Center for Computational Physics, University of Tsukuba, Japan. Collaborators Nozomu KAWAKATSU Masao MORI Jun’ichi SATO. Black Hole-Bulge Correlation. 1. BH-Bulge Mass Relation

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Masayuki UMEMURA Center for Computational Physics, University of Tsukuba, Japan

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  1. A Coevolution Scheme for Supermassive Black Holes and Galactic Bulges Masayuki UMEMURA Center for Computational Physics, University of Tsukuba, Japan Collaborators Nozomu KAWAKATSU Masao MORI Jun’ichi SATO

  2. Black Hole-Bulge Correlation 1. BH-Bulge Mass Relation  MBH /Mbulge  0.001 (Kormendy & Richstone 1995; Richstone 1995; Magorrian et al. 1998; Merrifield et al. 2000; Kormendy 2000; Merritt & Ferrarese 2001)  MBHMbulge1.53 MBH /Mbulge  0.005(MV-22) ; MBH /Mbulge  0.0005 (MV-18) (Laor 2001) MBH- Relation MBH, =4.72 (Ferrarese & Merritt 2000; Merrit & Ferrarese 2000) MBH, =3.75 (Gebhardt et al. 2000) MBH, =4.02±0.32 (Tremaine et al. 2002) MBH /Mdisk  0.005 for Disk component (Salucci et al. 2000; Sarzi et al. 2000) 2. 3.

  3. Why does SMBH mass linearly correlate with bulge mass ? What is the basic physics to determine MBH /Mbulge  O(10-3)? Present Prediction ( = 0.007 : H  He nuclear fusion energy conversion efficiency) Richstone 1995

  4. Angular Momentum Extraction Relativistic Radiation Hydrodynamics (Umemura et al. 1997; Fukue et al. 1997; Umemura et al. 1998) e.g. Poynting-Robertson effect in solar system

  5. Momentum loss Sato & Umemura, in preparation radiation field velocity cold gas

  6. SMBH Formation by Radiation Drag in Bulge Umemura, 2001, ApJ, 560, L29 Kawakatsu & Umemura, 2002, MNRAS, 329, 572 Angular Momentum Extraction Bulge L* photon number conservation (: optical depth by dust) R Mass Accretion Rate MDO (Massive Dark Object)

  7. Optically-Thick Regime Mass Accretion Rate Radiation Drag Time-Scale Mass of MDO

  8. Mass Accretion by Radiation Drag MDO-Bulge Mass Ratio ( = 0.007,  = net stellar conversion eficiency)

  9. BH Growth Radiation Drag Growth M L=LEdd MMDO Eddington Growth MBH t tcross

  10. SMBH to Bulge Mass Correlation Present Prediction

  11. Rees Diagram (1984) radiation drag

  12. MBH- Relation

  13. MBH- Relation Present Prediction Tremaine et al. 2002

  14. Why small BHs in disks?  Disks without AGNs  Sy1s  Sy2s  NLSy1s 0.03 0.1 1 Kawakatu & Umemura 2003 submitted to ApJ

  15. Geometrical Dilution of Radiation Fields Elliptical Galaxies Disk Galaxies low drag efficiency high drag efficiency

  16. Sy1 with Starburst  NLS1s Sy2 with starburst  Disks without AGNs  Sy1s  Sy2s  NLSy1s Present Prediction 0.03 0.1 1

  17. Coevolution of SMBHs and Bulges  SMBHs have been thought to be the central engine of AGNs. z=6.3 QSO  tBH109yr  QSO hosts are mostly luminous, well evolved elliptical galaxies.  Recently, the demography of galactic centers have shown a tight correlation between SMBHs and galactic bulges. The formation and evolution of SMBH, bulge, and QSO are mutually related.

  18. Mbulge(star) MBH MMDO L* ULIRG QSO LLAGN >1 <1 LAGN tw tcross(109-10yr) t • There is time delay between L* and LAGN. LAGN/L* increases until tcross . • LAGN is peaked around tcross.(QSO phase) • MBH /Mbulge increases with LAGN or age until tcross .

  19. Radiation Hydrodynamic Growth of BH via Radiation Drag + Chemical Evolution of Bulge PEGASE(Foic & Rocca-Volmerange 1997) Evolutionary spectral synthesis code Kawakatu, Umemura & Mori, 2003, ApJ, 583, 85

  20. Optical Depth Evolution Galactic wind 100 10 U B 1 V  K 0.1 0.01 0.001 Time [yr]

  21. Luminosity Evolution >1 <1 Galactic wind Luminosity [L] LLAGN ULIRG QSO Proto-QSO Time [yr] • LAGN /Lbulgeexhibits a AGN-dominant peak around 109yr. (QSO phase) • QSO phase is preceded by an optically thin, host-dominant “proto-QSO” phase. • Proto-QSO phase is preceded by an optically thick, host-dominant phase. (ULIRGs)

  22. Emission Line Width (Kaspi et al.1997; Loar et al. 1997; Peterson et al. 2000) 5000 <1 >1 1500 1000 vBLR[km/s] ULIRG LLAGN QSO Proto-QSO 100 Time [yr]  In Proto-QSO phase, the width of broad emission lines is less than 1500km/s. Proto-QSO = NLQSO1 = Growing BH phase

  23. “ACoevolution Scheme for SMBHs and Galactic Bulges“ Proto-QSO QSO LBG ULIRG LLAGN <1 <1 >1 <1 <1 Bulge enshrouded BH Type 2 QSO Nucleus 10-100 pc growing BH time

  24. Summary on BH Formation • MBH /Mbulge  0.14  =0.001: Radiation drag growth (key physics: =0.007) • MBH - Relation: CDM spectrum • MBH /Mbulge  0.005 for Disks: Geometrical dilution

  25. Summary on Coevolution • LAGN /Lbulgeexhibits a AGN-dominant peak around 109yr. (QSO phase) MBH /Mbulge  10-4-10-3 in QSO phase (key physics:  = 0.007) • QSO phase is preceded by a host-dominant “proto-QSO” phase. MBH /Mbulge < 10-5 -10-4 in proto-QSO (growing BH phase) Proto-QSOs are narrow line QSOs. Their properties are similar to those of high redshift radio galaxies. • Proto-QSO phase is preceded by an optically thick, host-dominant phase. (ULIRGs)

  26. Thank you for attention

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