The central black hole masses and Doppler factors of the <i>γ</i>-ray 
loud blazars

Fan, J. H.; GZ, Xie; Bacon, Roland

doi:10.1051/aas:1999194

Cited by 80 publications

(48 citation statements)

References 43 publications

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“…Therefore we think it is quite possible that Mrk 501 hosts a supermassive black hole with mass of about (1∼3)×10 9 M . We note that this is much larger than the maximum primary black hole mass (10 8 M ) required for the binary black hole model of Mrk 501 (Rieger & Mannheim 2000) and the mass (∼10 7 M ) estimated from the γ-ray variability timescale (Fan et al 1999). …”

Section: Bl Lac Objectsmentioning

confidence: 67%

Supermassive black hole masses of AGNs with elliptical hosts

Liu

Zhang

2002

A&A

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Abstract.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 10 7.5 M to 10 9 M . 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.

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Section: Bl Lac Objectsmentioning

confidence: 67%

Supermassive black hole masses of AGNs with elliptical hosts

Liu

Zhang

2002

A&A

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“…The shock-in-jet model, the most frequently cited model used to explain the IDVs, is based on a relativistic shock propagating down a jet and interacting with a highly non-uniform portion The variability timescales were defined in different ways. The doubling timescale is usually used to estimate the variability timescale of the large amplitude change in gamma rays (e.g., Fan et al 1999). A fast variability in the VHE gamma rays shows doubling times ∼ 15 minutes for Mrk 501 (Ahnen et al 2016).…”

Section: Discussionmentioning

confidence: 99%

Search for Intra-day Optical Variability in Mrk 501

Feng

Liu

Fan

et al. 2017

ApJ

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“…The correlation between γ-rays and radio bands suggests a strong beaming effect in γ-rays (Dondi & Ghisellini 1995;Fan et al 1998;Huang et al 1999;Cheng et al 2000;Fan et al 2016a), and the beaming factors (or Doppler factors) are estimated for some γ-ray loud blazars based on their rapid γ-ray variability time scale, X-ray and γ-ray emissions ( Mattox et al 1993, von Montigny et al 1995, Cheng, et al 1999Fan et al 1999;2013;2014;Fan 2005 ). In addition, a useful method to estimate Doppler factors may be found in a work (Lähteenimäki & Valtaoja 1999), followed by many other works (Fan et al 2009;Hovatta et al 2009;Lister et al 2009a;Savolainen et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Intrinsic Correlations for Flaring Blazars Detected by Fermi

Jiang

Yang

Xiao

et al. 2017

ApJL

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Blazars are an extreme subclass of active galactic nuclei. Their rapid variability, luminous brightness, superluminal motion, and high and variable polarization are probably due to a beaming effect. However, this beaming factor (or Doppler factor) is very difficult to measure. Currently, a good way to estimate it is to use the time scale of their radio flares. In this Letter, we use multiwavelength data and Doppler factors reported in the literatures for a sample of 86 flaring blazars detected by Fermi to compute their intrinsic multiwavelength data and intrinsic spectral energy distributions, and investigate the correlations among observed and intrinsic data. Quite interestingly, intrinsic data show a positive correlation between luminosity and peak frequency, in contrast with the behavior of observed data, and a tighter correlation between γ-ray luminosity and the lower energy ones. For flaring blazars detected by Fermi, we conclude that (1) Observed emissions are strongly beamed; (2) The anti-correlation between luminosity and peak frequency from the observed data is an apparent result, the correlation between intrinsic data being positive; and (3) Intrinsic γ-ray luminosity is strongly correlated with other intrinsic luminosities.

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The central black hole masses and Doppler factors of the γ-ray loud blazars

Cited by 80 publications

References 43 publications

Supermassive black hole masses of AGNs with elliptical hosts

Supermassive black hole masses of AGNs with elliptical hosts

Search for Intra-day Optical Variability in Mrk 501

Intrinsic Correlations for Flaring Blazars Detected by Fermi

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