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Weighing black holes in radio-loud AGNs Xue-Bing Wu ( 吳學兵 ) (Dept. of Astronomy, Peking Univ.) Collaborators: Ran Wang, F.K. Liu (PKU);

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Presentation on theme: "Weighing black holes in radio-loud AGNs Xue-Bing Wu ( 吳學兵 ) (Dept. of Astronomy, Peking Univ.) Collaborators: Ran Wang, F.K. Liu (PKU);"— Presentation transcript:

1 Weighing black holes in radio-loud AGNs Xue-Bing Wu ( 吳學兵 ) (Dept. of Astronomy, Peking Univ.) Collaborators: Ran Wang, F.K. Liu (PKU); M.Z. Kong, J.L. Han (NAOC)

2 Content zIntroduction zBH mass from the BLR size - emission line luminosity relation zBH mass from the fundamental plane relation of AGN elliptical hosts zSummary

3 1. Introduction zMost AGNs in Reverberation mapping studies are radio quiet. Can the R-L relation be applied to (extremely) radio- loud AGNs? zFor blazar-type AGNs, the emission line is weak/absent. How to estimate the BH mass of them?

4 BLR Scaling with Luminosity r  L 0.6±0.1 R-L relation from reverberation mapping r  L 1/2 With the R-L relation, we can estimate the BLR size from the optical continuum luminosity R-L relation from photoionization model (Kaspi et al. 2000, 2005)

5 SMBH and Galactic Bulge Relations of black hole mass with bulge luminosity and central velocity dispersion (for normal galaxies & AGNs) Ferrarese et al. (2001) AGN With the M-σ relation, we can estimate the BH mass from the stellar velocity dispersion

6 BH Mass from the R-L H  relation 2. BH Mass from the R-L H  relation (Wu, Wang, Kong, Liu & Han 2004, A&A, 424, 793) BLR sizes are usually derived from an empirical relation R  L 5100A 0.7 (Kaspi et al. 2000, 2005). Optical jets of some AGNs have been observed by the HST (Scarpa et al. 1999; Jester 2003; Parma et al. 2003). Optical Synchrotron radiations have been found in some RL AGNs (Whiting et al. 2001; Chiaberge et al. 2002; Cheung et al. 2003)

7 For RL AGNs, optical continuum luminosity may be significantly contributed from jets, and may not be a good indicator of ionizing luminosity It may be better to use the relation between the emission line luminosity and the BLR size

8 theR-L H  relationUsing the R-L 5100A relation one can overestimate M BH for extremely radio-loud quasars; using the R-L H  relation may be more accurate.

9 Recently we also extend such a study to UV broad emission lines (Mg II & CIV) (Kong, Wu, Wang, & Han, 2006, ChJAA, 6, 396)

10 BH mass of a blazar AO (Liu, Zhao & Wu, 2006, ApJ, 650, 749) zR-L 5100A relation: 1.5 x 10 9 M  zR-L H  relation: zR-L H  relation: 5.8 x 10 8 M  z  =FWHM[OII]/2.35 & M-σ relation: 3.6 x 10 8 M  zThe result from the R-L 5100A relation is overestimated z->BH mass of AO : 4.7 x 10 8 M 

11 Reverberation mapping can not apply to BL Lacs; Only a dozen of BL Lacs have measured  values (Falomo et al. 2002; Barth et al. 2002)Reverberation mapping can not apply to BL Lacs; Only a dozen of BL Lacs have measured  values (Falomo et al. 2002; Barth et al. 2002) Host galaxies of BL Lacs are ellipticals (Urry et al. 2000)Host galaxies of BL Lacs are ellipticals (Urry et al. 2000)  values can be derived from the fundamental plane of ellipticals  values can be derived from the fundamental plane of ellipticals (Bettoni et al. 2001) 3. BH Mass from the fundamental plane of AGN elliptical hosts (Wu, Liu & Zhang, 2002, A&A, 389, 742)

12 BH Mass from the fundamental plane of AGN elliptical hosts SMBH masses could be estimated for BL Lacs and other AGNs with high-quality HST images SMBH masses could be estimated for BL Lacs and other AGNs with high-quality HST images

13 Comparison of Eddington ratios of AGNs Comparison of Eddington ratios of AGNs The Eddington ratios (dimensionless accretion rates) of radio galaxies are about two orders lower than those of quasars.

14 The host galaxy was marginally resolved of r e =0.72’’ and R-band absolute magnitude M R = (Heidt et al. 1999) Using the BH mass – bulge luminosity relation (McLure & Dunlop 2002), It gives M BH =4.6E8 solar masses. M BH -  Using the fundamental plane of elliptical hosts and the M BH -  relation, It gives M BH =3.2E8 solar masses.  M BH ~4E8 solar masses  Support the new binary BH model (Valtaoja et al 2000) Primary black hole mass of OJ 287 (Liu & Wu, 2002, A&A, 388, L48)

15 4. Summary M BH - BH mass of AGNs can be obtained by reverberation mapping, the M BH -  relation and the R-L relation. heR BLR - emission line luminosity relation For (extremely) radio-loud AGNs, using the R-L 5100A relation may overestimate the BH mass. The R BLR - emission line luminosity relation is more preferable. the fundamental plane of their elliptical hostsM BH -  For blazar-type AGNs with weak/no emission lines, we can estimate the BH mass from the fundamental plane of their elliptical hosts and the M BH -  relation These methods can be applied to high-z quasars


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