SUPERMASSIVE BLACK HOLE MASSES FOR BLAZARS

2008 ◽  
Vol 17 (07) ◽  
pp. 1087-1093
Author(s):  
JUN-HUI FAN ◽  
YU-HAI YUAN ◽  
JIANG-SHUI ZHANG ◽  
JIANG-HE YANG
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Black Hole Mass ◽  
Central Black Hole ◽  
Supermassive Black Hole ◽  
Γ Ray ◽  
The Masses ◽  
Black Hole Masses ◽  
Two Temperature

In this work, we determine the central black hole mass for a sample of blazars including 30 γ-ray loud blazars with available variability timescales. The γ-ray energy, the emission size and the property of a two-temperature accretion disk are used to determine the absorption depth. If we take the intrinsic γ-ray luminosity to be λ times the Eddington luminosity, i.e. [Formula: see text], then we have following results: the masses of the black hole are in the range of 0.59 ~ 67.99 × 107M⊙(λ = 1.0) or 0.90 ~ 104.13 × 107M⊙(λ = 0.1). Blazars are also discussed.

scholarly journals Center Black Hole Mass Determinations for Fermi Blazars

2012 ◽  
Vol 8 (S290) ◽  
pp. 209-210
Author(s):  
J. H. Fan ◽  
Y. Liu ◽  
J. H. Yang ◽  
Y. H. Yuan ◽  
Y. Li ◽  
...  
Keyword(s):  
Black Hole ◽  
Time Scales ◽  
Black Hole Mass ◽  
Central Black Hole ◽  
Γ Ray ◽  
Black Hole Masses

AbstractIn this paper, we estimated the black hole mass for some blazars with available variability time scales by assuming that the γ-ray emissions are from a distance of 200Rg from the center. The results show that the central black hole masses are in the range of log (M/M⊙) = 6.45 to 8.30.

scholarly journals Central black hole mass determination for blazars

2007 ◽  
Vol 3 (S245) ◽  
pp. 243-244 ◽  
Author(s):  
J. H. Fan ◽  
Y. H. Yuan ◽  
Y. Huang ◽  
Y. Gao ◽  
T. X. Hua ◽  
...  
Keyword(s):  
Black Hole ◽  
Mass Determination ◽  
Black Hole Mass ◽  
Central Black Hole ◽  
Propagation Angle ◽  
Γ Ray ◽  
The Masses

AbstractIn this paper, we used the method to determine the central black mass (M), and the boosting factor (δ), the propagation angle (Φ), and the distance along the axis to the site of the γ-ray production (d) as well for 32 γ-ray loud blazars with available variability timescales. If we take the intrinsic γ-ray luminosity to be λ times the Eddington luminosity, i.e. $L_{\gamma}^{in}=\lambda{L_{\hbox{\it \scriptsize Edd}}}$, then we have following results: the masses of the black hole are in the range of (0.9 ~ 101)×107M⊙(λ = 1.0) or (1.30 ~ 153)×107M⊙(λ=0.1).

scholarly journals Estimating black hole masses: Accretion disk fitting versus reverberation mapping and single epoch

2020 ◽  
Vol 640 ◽  
pp. A39
Author(s):  
Samuele Campitiello ◽  
Annalisa Celotti ◽  
Gabriele Ghisellini ◽  
Tullia Sbarrato
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Good Description ◽  
Mapping Technique ◽  
Black Hole Mass ◽  
Reverberation Mapping ◽  
Fitting Procedure ◽  
Single Epoch ◽  
The Masses ◽  
Black Hole Masses

We selected a sample of 28 Type 1 active galactic nuclei for which a black hole mass has been inferred using the reverberation mapping technique and single epoch scaling relations. All 28 sources show clear evidence of the “Big Blue Bump” in the optical-UV band whose emission is produced by an accretion disk (AD) around a supermassive black hole. We fitted the spectrum of these sources with the relativistic thin AD model KERRBB in order to infer the black hole masses and compared them with those from Reverberation mapping and Single epoch methods, discussing the possible uncertainties linked to such a model by quantifying their weight on our results. We find that for the majority of the sources, KERRBB is a good description of the AD emission for a wide wavelength range. The overall uncertainty on the black hole mass estimated through the disk fitting procedure is ∼0.45 dex (which includes the uncertainty on fitting parameters such as e.g., spin and viewing angle), comparable to the systematic uncertainty of reverberation mapping and single epoch methods; however, such an uncertainty can be ≲0.3 dex if one of the parameters of the fit is well constrained. Although all of the estimates are affected by large uncertainties, the masses inferred using the three methods are compatible if the dimensionless scale factor f (linked to the unknown kinematics and geometry of the Broad Line Region) is assumed to be larger than one. For the majority of the sources, the comparison between the results coming from the three methods favors small spin values. To check the goodness of the KERRBB results, we compared them with those inferred with other models, such as AGNSED, a model that also accounts for the emission originating from an X-ray corona: using two sources with a good data coverage in the X band, we find that the masses estimated with the two models differ at most by a factor of ∼0.2 dex.

scholarly journals Time lags between starburst and AGN activity in galaxy mergers

2013 ◽  
Vol 9 (S303) ◽  
pp. 379-381
Author(s):  
M. Blank ◽  
W. J. Duschl
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Velocity Dispersion ◽  
Time Lag ◽  
Time Lags ◽  
Galaxy Mergers ◽  
Black Hole Mass ◽  
Central Black Hole ◽  
Stellar Velocity ◽  
Flow Through

AbstractWe show that the observed time lag between starburst and AGN activity can be explained by a viscous time lag the gas needs to flow through the AGN's accretion disk before reaching the central black hole. Our calculations reproduce the observed time lag and are in agreement with the observed correlation between black hole mass and stellar velocity dispersion.

scholarly journals Growing Supermassive Black Holes Inside Cosmological Simulations

2009 ◽  
Vol 5 (S267) ◽  
pp. 333-333
Author(s):  
Robyn Levine ◽  
Nickolay Y. Gnedin ◽  
Andrew J. S. Hamilton
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Accretion Disk ◽  
Adaptive Mesh Refinement ◽  
Adaptive Mesh ◽  
Outer Edge ◽  
Central Black Hole ◽  
Supermassive Black Hole ◽  
Circumnuclear Disk

Using a hydrodynamic adaptive mesh refinement code, we simulate the growth and evolution of a typical disk galaxy hosting a supermassive black hole (SMBH) within a cosmological volume. The simulation covers a dynamical range of 10 million, which allows us to study the transport of matter and angular momentum from super-galactic scales down to the outer edge of the accretion disk around the SMBH. A dynamically interesting circumnuclear disk develops in the central few hundred parsecs of the simulated galaxy, through which gas is stochastically transported to the central black hole.

scholarly journals Wandering of the central black hole in a galactic nucleus and correlation of the black hole mass with the bulge mass

2021 ◽  
Author(s):  
Hajime Inoue
Keyword(s):  
Black Hole ◽  
Loss Rate ◽  
Energy Gain ◽  
Stellar Disk ◽  
Black Hole Mass ◽  
Central Black Hole ◽  
Massive Black Hole ◽  
Stellar Cluster ◽  
Upper Limit ◽  
Simple Parameter

Abstract We investigate a mechanism for a super-massive black hole at the center of a galaxy to wander in the nucleus region. A situation is supposed in which the central black hole tends to move by the gravitational attractions from the nearby molecular clouds in a nuclear bulge but is braked via the dynamical frictions from the ambient stars there. We estimate the approximate kinetic energy of the black hole in an equilibrium between the energy gain rate through the gravitational attractions and the energy loss rate through the dynamical frictions in a nuclear bulge composed of a nuclear stellar disk and a nuclear stellar cluster as observed from our Galaxy. The wandering distance of the black hole in the gravitational potential of the nuclear bulge is evaluated to get as large as several 10 pc, when the black hole mass is relatively small. The distance, however, shrinks as the black hole mass increases, and the equilibrium solution between the energy gain and loss disappears when the black hole mass exceeds an upper limit. As a result, we can expect the following scenario for the evolution of the black hole mass: When the black hole mass is smaller than the upper limit, mass accretion of the interstellar matter in the circumnuclear region, causing the AGN activities, makes the black hole mass larger. However, when the mass gets to the upper limit, the black hole loses the balancing force against the dynamical friction and starts spiraling downward to the gravity center. From simple parameter scaling, the upper mass limit of the black hole is found to be proportional to the bulge mass, and this could explain the observed correlation of the black hole mass with the bulge mass.

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