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Parsec-Scale Jets and Tori in Seyfert Galaxies

Published online by Cambridge University Press:  13 May 2016

A.L. Roy ,
J.M. Wrobel ,
A.S. Wilson ,
J.S. Ulvestad ,
R.P. Norris ,
C.G. Mundell ,
T.P. Krichbaum ,
H. Falcke  and
E. J. M. Colbert
A.L. Roy
Affiliation:
MPIfR, Bonn, Germany, [email protected]
J.M. Wrobel
Affiliation:
NRAO, PO Box O, Socorro, NM 87801, USA
A.S. Wilson
Affiliation:
University of Maryland, College Park, MD 20742, USA
J.S. Ulvestad
Affiliation:
NRAO, PO Box O, Socorro, NM 87801, USA
R.P. Norris
Affiliation:
ATNF, PO Box 76, Epping NSW 1710, Australia
C.G. Mundell
Affiliation:
ARI, Liverpool John Moores University, Birkenhead, UK
T.P. Krichbaum
Affiliation:
MPIfR, Bonn, Germany, [email protected]
H. Falcke
Affiliation:
MPIfR, Bonn, Germany, [email protected]
E. J. M. Colbert
Affiliation:
JHU, Dept Physics and Astronomy, Baltimore, MD 21218, USA

Abstract

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What causes the dichotomy between very powerful and very weak radio emission from AGNs? Perhaps the engines are the same but the jets get disrupted by dense ISM in radio-quiet objects, or else the engines are intrinsically different with jet power scaling with, say, black hole spin. To distinguish, one can look for interaction between the jets and the NLR and measure the jet speed close to the core using VLBI, before environmental effects become important. We find that in radio-quiet AGN, the jets appear slower and have a greater tendency to bend, and that one-sidedness and flat-spectrum cores are probably due to obscuration.

Type
The Inner Regions of Galaxies
Information
Symposium - International Astronomical Union , Volume 205: Galaxies and their Constituents at the Highest Angular Resolutions , 2001 , pp. 70 - 71
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

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