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What makes a galaxy radio-loud?

Published online by Cambridge University Press:  17 August 2012

R. A. Ortega-Minakata ,
J. P. Torres-Papaqui ,
H. Andernach ,
R. Coziol ,
J. M. Islas-Islas ,
I. Plauchu-Frayn ,
D. M. Neri-Larios  and
M. del C. Rojas-Granados
R. A. Ortega-Minakata
Affiliation:
Departamento de Astronomía, Universidad de Guanajuato, C.P. 36000, Guanajuato, Mexico email: [email protected]
J. P. Torres-Papaqui
Affiliation:
Departamento de Astronomía, Universidad de Guanajuato, C.P. 36000, Guanajuato, Mexico email: [email protected]
H. Andernach
Affiliation:
Departamento de Astronomía, Universidad de Guanajuato, C.P. 36000, Guanajuato, Mexico email: [email protected]
R. Coziol
Affiliation:
Departamento de Astronomía, Universidad de Guanajuato, C.P. 36000, Guanajuato, Mexico email: [email protected]
J. M. Islas-Islas
Affiliation:
Departamento de Astronomía, Universidad de Guanajuato, C.P. 36000, Guanajuato, Mexico email: [email protected]
I. Plauchu-Frayn
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC), E-18008, Granada, Spain
D. M. Neri-Larios
Affiliation:
Departamento de Astronomía, Universidad de Guanajuato, C.P. 36000, Guanajuato, Mexico email: [email protected]
M. del C. Rojas-Granados
Affiliation:
División de Ingenierías, Universidad de Guanajuato, C.P. 36885, Salamanca, Mexico
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Abstract

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We compare the Spectral Energy Distribution (SED) of radio-loud and radio-quiet AGNs in three different samples observed with SDSS: radio-loud AGNs (RLAGNs), Low Luminosity AGNs (LLAGNs) and AGNs in isolated galaxies (IG-AGNs). All these galaxies have similar optical spectral characteristics. The median SED of the RLAGNs is consistent with the characteristic SED of quasars, while that of the LLAGNs and IG-AGNs are consistent with the SED of LINERs, with a lower luminosity in the IG-AGNs than in the LLAGNs. We infer the masses of the black holes (BHs) from the bulge masses. These increase from the IG-AGNs to the LLAGNs and are highest for the RLAGNs. All these AGNs show accretion rates near or slightly below 10% of the Eddington limit, the differences in luminosity being solely due to different BH masses. Our results suggests there are two types of AGNs, radio quiet and radio loud, differing only by the mass of their bulges or BHs.

Keywords

galaxies: activegalaxies: evolutiongalaxies: fundamental parametersgalaxies: statisticsradio continuum: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S284: The Spectral Energy Distribution of Galaxies , September 2011 , pp. 221 - 223
Copyright
Copyright © International Astronomical Union 2012

References

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