Issue |
A&A
Volume 389, Number 3, July III 2002
|
|
---|---|---|
Page(s) | 742 - 751 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20020577 | |
Published online | 01 July 2002 |
Supermassive black hole masses of AGNs with elliptical hosts
National Astronomical Observatories of CAS & Department of Astronomy, Peking University, Beijing 100871, PR China e-mail: wuxb@bac.pku.edu.cn; fkliu@bac.pku.edu.cn; bzty@bac.pku.edu.cn
Corresponding author: Xue-Bing Wu, wuxb@bac.pku.edu.cn
Received:
4
February
2002
Accepted:
8
March
2002
The recently discovered tight correlation between supermassive black hole mass and
central velocity dispersion for both inactive and
active galaxies suggests a possibility to estimate the
black hole mass from the measured central velocity dispersion. However, for
most AGNs it is difficult to measure the central velocity dispersions of their
host galaxies directly with spectroscopic studies. In this paper
we adopt the
fundamental plane for ellipticals to estimate the central velocity
dispersion and black hole mass for a number of AGNs with morphology
parameters of their elliptical host galaxies obtained by the Hubble Space
Telescope imaging observations.
The estimated black hole masses of 63 BL Lac objects, 10 radio galaxies,
10 radio-loud quasars and 9 radio-quiet quasars are mostly in the range of
to
. No significant difference in black hole
mass is found for high-frequency peaked BL Lacs and low-frequency peaked
BL Lacs, as well as for radio galaxies and radio-loud quasars.
The Eddington ratios of radio galaxies are
substantially smaller than those of quasars.
This
suggests that the different observational features of these radio-loud AGNs may be
mainly dominated by different accretion rate rather than by
the black hole mass, which is in agreement with some evolutionary scenarios recently
proposed for radio-loud AGNs.
Different to some previous claims,
we found that the derived mean black hole mass for radio-loud quasars is only
slightly larger than that of radio-quiet quasars. Though the black hole mass
distributions between radio-loud and radio-quiet quasars are statistically
different, their Eddington ratio distributions are probably from the same population.
In addition, we noted that the relation
between black hole mass and host galaxy luminosity we obtained
using the fundamental plane
provides further arguments for a nonlinear scaling law between
supermassive black hole mass and galactic bulge mass.
Key words: black hole physics / BL Lacertae objects: general / galaxies: active / galaxies: nuclei / quasars: general
© ESO, 2002
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