Supermassive black hole masses in type II active galactic  nuclei with
polarimetric broad emission lines

AbstractUsing the recent ROGUE I catalogue of galaxies with radio cores (Kozie_l-Wierzbowska et al. 2020) and after selecting the objects which are truly radio active galactic nuclei, AGNs, (which more than doubles the samples available so far), we perform a thorough comparison of the properties of radio galaxies with and without optical emission lines (galaxies where the equivalent width of Hα is smaller than 3Å are placed in the last category). We do not find any strong dichotomy between the two classes as regards the radio luminosities or black hole masses. The same is true when using the common classification into high- and low-excitation radio galaxies (HERGs and LERGs respectively).

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The First Supermassive Black Hole Mass Measurement in Active Galactic Nuclei Using the Polarization of Broad Emission Line Mg ii

The Astrophysical Journal ◽

10.3847/2041-8213/ac2d30 ◽

2021 ◽

Vol 921 (1) ◽

pp. L21

Author(s):

Đorđe V. Savić ◽

Luka Č. Popović ◽

Elena Shablovinskaya

Keyword(s):

Black Hole ◽

Emission Line ◽

Active Galactic Nuclei ◽

Mass Measurement ◽

Galactic Nuclei ◽

Black Hole Mass ◽

Supermassive Black Hole ◽

Broad Emission ◽

Broad Emission Line

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Black Hole Masses and Unification of Seyferts

Symposium - International Astronomical Union ◽

10.1017/s0074180900162163 ◽

1999 ◽

Vol 194 ◽

pp. 311-312

Author(s):

R. Bachev ◽

G. T. Petrov ◽

L. Slavcheva ◽

B. Mihov

Keyword(s):

Black Hole ◽

Active Galactic Nuclei ◽

Galactic Nuclei ◽

Power Source ◽

Active Galaxies ◽

Supermassive Black Hole ◽

Central Engine ◽

Internal Structures ◽

Accretion Rates ◽

Black Hole Masses

The most commonly invoked power source of Active Galactic Nuclei (AGN) is accretion of galactic gas (probably through a disk) onto a supermassive black hole in the center of the nucleus (Rees 1984). As is well known, a black hole is completely defined by its mass and angular momentum. The unification scheme of active galaxies assumes that two known Seyfert types (Sy1 and Sy2) are not intrinsically different, i. e. their black hole masses, accretion rates and the whole internal structures are identical (Antonucci 1993) and observed differences are due just to a different orientation to the observer of the axisymmetrical central structure (central engine, BLR and thick torus, shadowing broad lines from some directions).

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Hydrodynamics Near the Central Engine

International Astronomical Union Colloquium ◽

10.1017/s0252921100086176 ◽

1986 ◽

Vol 89 ◽

pp. 369-383

Author(s):

John F. Hawley

Keyword(s):

Black Hole ◽

Active Galactic Nuclei ◽

Galactic Nuclei ◽

Disk Formation ◽

Accretion Flows ◽

Supermassive Black Hole ◽

Central Engine ◽

Accretion Rates ◽

Considerable Work ◽

Black Hole Masses

AbstractThe “central engine” of quasars and active galactic nuclei Is most likely powered by accretion into a supermassive black hole. A menagerie of steady state accretion flows have been developed, and these are briefly reviewed. Several examples from recent numerical calculations of axisymmetric accretion flows provide disk formation scenarios from which one can calculate plasma densities, and other values of interest for a range of accretion rates and black hole masses. These results can be compared with the well studied, but physically unrealistic case of radial accretion. Although a reasonable conceptual picture of the central engine has been developed, considerable work remains to be done.

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