Stellar Velocity Dispersion and Black Hole Mass in the Blazar Markarian 501

2002 ◽  
Vol 566 (1) ◽  
pp. L13-L16 ◽  
Author(s):  
Aaron J. Barth ◽  
Luis C. Ho ◽  
Wallace L. W. Sargent
Keyword(s):  
Black Hole ◽  
Velocity Dispersion ◽  
Black Hole Mass ◽  
Stellar Velocity

A LOCAL BASELINE OF THE BLACK HOLE MASS SCALING RELATIONS FOR ACTIVE GALAXIES. II. MEASURING STELLAR VELOCITY DISPERSION IN ACTIVE GALAXIES

2012 ◽  
Vol 201 (2) ◽  
pp. 29 ◽  
Author(s):  
Chelsea E. Harris ◽  
Vardha N. Bennert ◽  
Matthew W. Auger ◽  
Tommaso Treu ◽  
Jong-Hak Woo ◽  
...  
Keyword(s):  
Black Hole ◽  
Velocity Dispersion ◽  
Active Galaxies ◽  
Scaling Relations ◽  
Black Hole Mass ◽  
Mass Scaling ◽  
Stellar Velocity

scholarly journals Characterisation of the continuum and kinematical properties of nearby NLS1

2019 ◽  
Vol 629 ◽  
pp. A50
Author(s):  
Gabriel A. Oio ◽  
Luis R. Vega ◽  
Eduardo O. Schmidt ◽  
Diego Ferreiro
Keyword(s):  
Black Hole ◽  
Power Law ◽  
Velocity Dispersion ◽  
Spectral Synthesis ◽  
Sloan Digital Sky Survey ◽  
Black Hole Mass ◽  
Composite Spectra ◽  
Sky Survey ◽  
Stellar Velocity ◽  
Gaussian Decomposition

Aims. In order to study the slope and strength of the non-stellar continuum, we analysed a sample from nearby Narrow Line Seyfert 1 (NLS1). Also, we re-examined the location of NLS1 galaxies on the MBH − σ⋆ relation, using the stellar velocity dispersion and the [OIII]λ5007 emission line as a surrogate of the former. Methods. We studied spectra of a sample of 131 NLS1 galaxies taken from the Sloan Digital Sky Survey (SDSS) DR7. We approached determining the non-stellar continuum by employing the spectral synthesis technique, which uses the code STARLIGHT, and by adopting a power-law base to model the non-stellar continuum. Composite spectra of NLS1 galaxies were also obtained based on the sample. In addition, we obtained the stellar velocity dispersion from the code and by measuring Calcium II Triplet absorption lines and [OIII] emission lines. From Gaussian decomposition of the Hβ profile we calculated the black hole mass. Results. We obtained a median slope of β = −1.6 with a median fraction of contribution of the non-stellar continuum to the total flux of 0.64. We determined black hole masses in the range of log(MBH/M⊙) = 5.6–7.5, which is in agreement with previous works. We found a correlation between the luminosity of the broad component of Hβ and black hole mass with the fraction of a power-law component. Finally, according to our results, NLS1 galaxies in our sample are located mostly underneath the MBH − σ⋆ relation, both considering the stellar velocity dispersion (σ⋆) and the core component of [OIII]λ5007.

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 STELLAR VELOCITY DISPERSION MEASUREMENTS IN HIGH-LUMINOSITY QUASAR HOSTS AND IMPLICATIONS FOR THE AGN BLACK HOLE MASS SCALE

2013 ◽  
Vol 773 (2) ◽  
pp. 90 ◽  
Author(s):  
C. J. Grier ◽  
P. Martini ◽  
L. C. Watson ◽  
B. M. Peterson ◽  
M. C. Bentz ◽  
...  
Keyword(s):  
Black Hole ◽  
Velocity Dispersion ◽  
Mass Scale ◽  
Black Hole Mass ◽  
High Luminosity ◽  
Stellar Velocity

scholarly journals THE BLACK HOLE MASS–STELLAR VELOCITY DISPERSION RELATION OF NARROW-LINE SEYFERT 1 GALAXIES

2015 ◽  
Vol 801 (1) ◽  
pp. 38 ◽  
Author(s):  
Jong-Hak Woo ◽  
Yosep Yoon ◽  
Songyoun Park ◽  
Daeseong Park ◽  
Sang Chul Kim
Keyword(s):  
Black Hole ◽  
Dispersion Relation ◽  
Velocity Dispersion ◽  
Narrow Line ◽  
Black Hole Mass ◽  
Stellar Velocity

scholarly journals The Black Hole Mass of BL Lacertae Objects from the Stellar Velocity Dispersion of the Host Galaxy

2002 ◽  
Vol 569 (1) ◽  
pp. L35-L38 ◽  
Author(s):  
R. Falomo ◽  
J. K. Kotilainen ◽  
A. Treves
Keyword(s):  
Black Hole ◽  
Velocity Dispersion ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Bl Lacertae Objects ◽  
Bl Lacertae ◽  
Stellar Velocity

scholarly journals The Megamaser Cosmology Project: precise black hole mass measurement and the implication for the MBH–σ∗ relation

2014 ◽  
Vol 10 (S312) ◽  
pp. 56-60
Author(s):  
Cheng-Yu Kuo ◽  
James A. Braatz ◽  
James J. Condon ◽  
Caterina M. V. Impellizzeri ◽  
Kwok-Yung Lo ◽  
...  
Keyword(s):  
Black Hole ◽  
Velocity Dispersion ◽  
Mass Measurement ◽  
Black Hole Mass ◽  
Mass Measurements ◽  
The North ◽  
Accuracy And Precision ◽  
The Galaxy ◽  
Stellar Velocity ◽  
Tight Correlation

AbstractWe made dynamical black hole mass measurements from nineteen Seyfert 2 galaxies which host sub-parsec H2O maser disks using the H2O megamaser technique. The nearly perfect Keplerian rotation curves in many of these maser systems guarantee the high accuracy and precision of the black hole mass measurements. With the stellar velocity dispersion (σ∗) of the galaxy bulges measured with the Dupont 2.5 m telescope at Las Campanas Observatory in the South and the Apache Point Observatory (APO) 3.5m telescope in the North, we found that H2O maser galaxies, most of which host pseudo bulges rather than classical bulges, do not all follow the MBH–σ∗ relation shown in the literature. This result is well consistent with the latest findings by Kormendy & Ho (2013) that only early type galaxies and galaxies with classical bulges follow a tight MBH–σ∗ relation. Such a tight correlation may not exist in pseudo bulge galaxies.

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