Issue |
A&A
Volume 436, Number 3, June IV 2005
|
|
---|---|---|
Page(s) | 799 - 804 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20034576 | |
Published online | 03 June 2005 |
The basic parameters of γ-ray-loud blazars
Center for Astrophysics, Guangzhou University, Guangzhou 510400, PR China e-mail: fjh@gzhu.edu.cn Chinese Academy of Science-Peking University Joint Beijing Astrophysical Center(CAS-PKU.BAC), Beijing, PR China National Astronomical Observatory, Chinese Academy of Sciences, Beijing, PR China
Received:
25
October
2003
Accepted:
4
January
2005
We determined the basic parameters, such as the central
black hole mass (M), the boosting factor (or Doppler factor) (δ), the propagation angle (Φ) and
the distance along the axis to the site of
γ-ray production (d) for 23 γ-ray-loud blazars
using their available variability timescales.
In this
method, the absorption effect depends on the γ-ray
energy, emission size and property of the accretion disk. Using
the intrinsic γ-ray luminosity as a fraction λ of
the Eddington luminosity, and
the optical depth equal to unity, we can determine the upper
limit of the central black hole masses. We found that the black
hole masses range between
and
when
and 1.0 are adopted. Since this method is
based on gamma-ray emissions and the short time-scale of the
sources, it can also be used for central black hole mass
determination of high redshift gamma-ray sources. In the case of
the upper limit of black hole mass there is no clear difference
between BLs and FSRQs, which suggests that the central black hole
masses do not play an important role in the evolutionary sequence
of blazars.
Key words: galaxies: quasars: general / galaxies: BL Lacertae objects: general / galaxies: jets / galaxies: nuclei
© ESO, 2005
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