Weighing black holes in radioloud AGNs

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Weighing black holes in radio-loud AGNs

• Xue-Bing Wu (???)
• (Dept. of Astronomy, Peking Univ.)
• wuxb_at_bac.pku.edu.cn
• Collaborators Ran Wang, F.K. Liu (PKU) M.Z.
  Kong, J.L. Han (NAOC)

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Content

• Introduction
• BH mass from the BLR size - emission line
  luminosity relation
• BH mass from the fundamental plane relation of
  AGN elliptical hosts
• Summary

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1. Introduction

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

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BLR Scaling with Luminosity
R-L relation from reverberation mapping
R-L relation from photoionization model
(Kaspi et al. 2000, 2005)
With the R-L relation, we can estimate the BLR
size from the optical continuum luminosity
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SMBH and Galactic Bulge

• Relations of black hole mass with bulge
  luminosity and central velocity dispersion (for
  normal galaxies AGNs)

AGN
Ferrarese et al. (2001)
With the M-s relation, we can estimate the BH
mass from the stellar velocity dispersion
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2. BH Mass from the R-LH? relation (Wu, Wang,
Kong, Liu Han 2004, AA, 424, 793)

• BLR sizes are usually derived from an empirical
  relation R? L5100A0.7(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)

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• 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

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• Using the R-L5100A relation one can overestimate
  MBH for extremely radio-loud quasars using the
  R-LH? relation may be more accurate.

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Recently we also extend such a study to UV broad
emission lines (Mg II CIV) (Kong, Wu, Wang,
Han, 2006, ChJAA, 6, 396)
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BH mass of a blazar AO 0235164(Liu, Zhao Wu,
2006, ApJ, 650, 749)

• R-L5100A relation 1.5 x 109 M?
• R-LH? relation 5.8 x 108 M?
• ?FWHMOII/2.35 M-s relation 3.6 x 108
  M?
• The result from the R-L5100A relation is
  overestimated
• -gtBH mass of AO 0235164 4.7 x 108 M?

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3. BH Mass from the fundamental plane of AGN
elliptical hosts (Wu, Liu Zhang, 2002, AA,
389, 742)

• 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)
• ? values can be derived from the fundamental
  plane of ellipticals

(Bettoni et al. 2001)
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• 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

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• Comparison of Eddington ratios of AGNs

The Eddington ratios (dimensionless accretion
rates) of radio galaxies are about two orders
lower than those of quasars.
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Primary black hole mass of OJ 287 (Liu Wu,
2002, AA, 388, L48)
The host galaxy was marginally resolved of
re0.72 and R-band absolute magnitude MR
-23.23 (Heidt et al. 1999) Using the BH mass
bulge luminosity relation (McLure Dunlop
2002), It gives MBH4.6E8 solar masses. Using
the fundamental plane of elliptical hosts and the
MBH - ? relation, It gives MBH3.2E8 solar
masses. ? MBH4E8 solar masses ? Support the new
binary BH model (Valtaoja et al 2000)
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4. Summary

• BH mass of AGNs can be obtained by reverberation
  mapping, the MBH - ? relation and the R-L
  relation.
• For (extremely) radio-loud AGNs, using the
  R-L5100A relation may overestimate the BH mass.
  The RBLR -emission line luminosity relation is
  more preferable.
• 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 MBH - ? relation
• These methods can be applied to high-z quasars