Black Hole Mass of Microquasars and Quasars

1. Black Hole Mass of Microquasars and Quasars Xue-Bing Wu wuxb@bac.pku.edu.cn (Dept. of Astronomy, Peking Univ.)

2. Content • Introduction • BH Mass of Microquasars • BH mass of AGNs • Relations of BH mass and other properties • Discussions

3. 1. Introduction • Similarities between microquasars and quasars • BH • Accretion Disk • Relativistic Jet • Radio Lobe • … • Advantages of studying microquasars • Nearby • Short timescale (t  MBH)

4. 2. BH mass of Microquasars • BH mass determinations • Kepler’s third law • Mass function • BH mass i c.m Ms Mp a

5. BH mass and QPO in BHXRBs(McClintock & Remillard 2003)

6. BH Masses of BHXRBs Cyg X-1 1915+105 1655-40 1550-564

7. Relation between HFQPO frequency and BH mass (McClintock & Remillard 2003) GRO J1655-40 f  1/MBH XTE J1550-564 GRS 1915+105

8. Mass determination is helpful to understand the nature of compact object and accretion process in XRBs NS BH McClintock et al. (2003)

9. 3. BH Mass of AGNs • 10^6 to 10^9 solar mass SMBH are needed to explain the energy output of AGNs • Stellar, gas and maser dynamics have been used to estimate the SMBH masses of some nearby galaxies, but can not be applied to most of AGNs • Reliable SMBH mass of AGN can be obtained by using the optical/UV reverberation mapping and some empirical relations (MBH- relation, RBLR-L5100A and RBLR-LH relations)

10. Reverberation mappingfrom optical variability • Broad line region size RBLR estimated by the time delay that corresponds to the light travel time between the continuum source and the line-emitting gas: RBLR =c  t • BLR velocity V estimatedby the FWHM of broad line • SMBH mass is estimated with (Peterson 1997) -- Both AGN continuum and broad emission line fluxes vary with time and there is a delay (days to months) between their variations.

11. Determination of Supermassive black hole masses of AGN with reverberation mapping Kaspi et al. (2000)

12. Empirical relation between RBLR & UV/optical continuum luminosity (Kaspi et al. 2000; Vestergaard 2002) SMBH mass of an AGN can be estimated from a single spectrum with the RBLR-L5100A relation !

13. SMBH in highest redshift quasar (z=6.4) Willott et al. (2003) Barth et al. (2003) FWHM(MgII)=5500km/s MBH=2E9 Msun FWHM(CIV)=9000km/s MBH=6E9 Msun FWHM(MgII)=6000km/s MBH=3E9 Msun

14. AGN Black Hole Mass estimation with the R-LH relation (Wu, Wang, Kong, Liu & Han 2004, A&A, in press) • For RL AGNs, optical continuum luminosity may be significantly contributed from jets, and may not be a good indicator of ionizing luminosity • Using the R-L5100A relation can overestimate MBH for radio-loud quasars • It may be better to use the relation between the emission line luminosity and the BLR size

15. Relations of black hole mass with bulge luminosity and central velocity dispersion (AGN too) (Ferrarese et al. 2001) MBH- relation provides another way to estimate the SMBH mass of AGNs

16. Estimating the SMBH Mass of AGN with elliptical host galaxy from the fundamental plane • (Wu, Liu & Zhang, 2002, A&A, 389, 742) • Reverberation mapping can not apply to BL Lacs; Only 10 BL Lacs have measured  values (Falomo et al. 2002; Barth et al. 2002) • Host galaxies of BL Lacs are ellipticals (Urry et al. 2000) •  values can be derived based on the fundamental plane of ellipticals; then SMBH masses could be estimated for BL Lacs with high-quality images (Bettoni et al. 2001)

17. Type 2 AGNs Type 2 AGNs Type 1 AGNs Type 1 AGNs Phenomenon: Phenomenon: BL Lac Objects BL Lac Objects Quiescent Galaxies Quiescent Galaxies Primary Methods: Primary Methods: Stellar, gas dynamics Stellar, gas dynamics Megamasers Megamasers 2-d RM 2-d RM 1-d RM 1-d RM Fundamental Empirical Relationships: Fundamental Empirical Relationships: MBH– * MBH– * AGNMBH– * AGNMBH– * Secondary Mass Indicators: Secondary Mass Indicators: Fundamental plane: e, re  * MBH Fundamental plane: e, re  * MBH [O III] line width V  * MBH Broad-line width V & size scaling with luminosity R  L0.7 MBH Summary: Methods of estimating SMBH Masses Summary: Methods of estimating SMBH Masses Low-z AGNs Low-z AGNs Peterson (2004) High-z AGNs High-z AGNs

18. 4. Relation of BH mass and other properties • BH mass and X-ray variability (τbreak MBH ?) NLS1 BLS1 McHardy et al. (2004), MNRAS

19. A fundamental plane of black hole activity • (Merloni et al. MNRAS, 2003)

20. 5. Discussions • Universal picture of microquasars and quasars ? • Likely. Accretion physics is the same • Can we estimate the BH mass from spectral fitting for both microquasars and quasars ? • Possible. However it is model dependent • Shrader & Titarchuk (2003): DiskBB+BMC model; A method is suggested to estimate MBH for BHXRB, NLS1 and ULX from X-ray spectral fitting

21. Shrader & Titarchuk (2003) BHXRB NLS1 ULX

22. Can we use HFQPO frequency to estimate the BH masses of ULXs and AGNs? • Possible. Abramowicz et al. (2004)

23. Can we see transient AGNs, similar as microquasars ? • Possible. Some have been found by ROSAT (Grupe 2002): IC 3599(Sy 2), WPVS007 (NLS1) • Do different types of AGNs correspond to BHXRBs in different spectral state? • Likely. NLS1s Seyfert 1s and RQQs Seyfert 2s, LINERs & RLQs Fender (2003)

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