scholarly journals Black hole masses from emission‐line widths

2021 ◽  
Author(s):  
Elena Dalla Bontà ◽  
Bradley M. Peterson
Keyword(s):  
Black Hole ◽  
Emission Line ◽  
Line Widths ◽  
Black Hole Masses

scholarly journals THE IMPORTANCE OF BROAD EMISSION LINE WIDTHS IN SINGLE-EPOCH BLACK HOLE MASS ESTIMATES

2012 ◽  
Vol 753 (1) ◽  
pp. L2 ◽  
Author(s):  
R. J. Assef ◽  
S. Frank ◽  
C. J. Grier ◽  
C. S. Kochanek ◽  
K. D. Denney ◽  
...  
Keyword(s):  
Black Hole ◽  
Emission Line ◽  
Black Hole Mass ◽  
Broad Emission ◽  
Line Widths ◽  
Broad Emission Line ◽  
Single Epoch

THE RELATIONSHIP AMONG XBLs, RBLs AND FSRQs

2010 ◽  
Vol 19 (06) ◽  
pp. 909-915
Author(s):  
HONG-GUANG WANG ◽  
JUN-HUI FAN ◽  
YONG HUANG ◽  
JING PAN ◽  
JIANG-HE YANG
Keyword(s):  
Black Hole ◽  
Emission Line ◽  
Central Black Hole ◽  
Bl Lacertae Objects ◽  
X Ray ◽  
Bolometric Luminosity ◽  
Bl Lacertae ◽  
Spectrum Radio ◽  
The Relationship ◽  
Black Hole Masses

In this work, we revisited the relationship between the subclasses of blazars (X–ray selected BL Lacertae objects (XBLs), radio selected BL Lacertae objects (RBLs), and flat spectrum radio quasars (FSRQs)) based on a sample of blazars. We found that the FSRQs–RBLs–XBLs relationship is clear in their bolometric luminosity, emission line luminosity and the accretion ratio with V FSRQs > V RBLs > V XBLs , where V stands for the three parameters. However, there is no clear difference amongst their central black hole masses. The bolometric luminosity is closely correlated with the emission line luminosity and the accretion ratio.

scholarly journals Metallicity and black hole masses of z≃6 quasars

2006 ◽  
Vol 2 (14) ◽  
pp. 257-257
Author(s):  
Jaron D. Kurk ◽  
Fabian Walter ◽  
Dominik Riechers ◽  
Hans-Walter Rix ◽  
Stefan Wagner ◽  
...  
Keyword(s):  
Black Hole ◽  
Nir Spectroscopy ◽  
Emission Lines ◽  
Line Widths ◽  
Black Hole Masses

AbstractWe present NIR spectroscopy of emission lines of a sample of five z≃6 quasars, including fainter objects than observed before. The measured FeII/MgII ratios are around solar and consistent with a lack of evolution of the metallicity of quasar BLRs up to z≃6, suggesting that stars in their hosts formed at z≫6. The BH masses, measured from both MgII and CIV line widths are within the range 2-16×108M⊙, the smallest found in such distant objects.

Estimating Black Hole Masses of AGNs using Ultraviolet Emission Line Properties

2006 ◽  
Vol 6 (4) ◽  
pp. 396-410 ◽  
Author(s):  
Min-Zhi Kong ◽  
Xue-Bing Wu ◽  
Ran Wang ◽  
Jin-Lin Han
Keyword(s):  
Black Hole ◽  
Emission Line ◽  
Ultraviolet Emission ◽  
Black Hole Masses
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