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Weak Radio Galaxies: Narrow-Band Optical Imaging

Published online by Cambridge University Press:  25 May 2016

René Carrillo  and
Irene Cruz-González
René Carrillo
Affiliation:
Instituto de Astronomía, UNAM Apdo. 70-264, México D.F., 04510, México
Irene Cruz-González
Affiliation:
Instituto de Astronomía, UNAM Apdo. 70-264, México D.F., 04510, México

Extract

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Previous studies show that: a) radio galaxies and radio-loud quasars have emission-line gas (ELG) which is extended on scales of tenths of kiloparsecs; b) there is convincing evidence that the kinematics and excitation of the very extended emission-line gas is governed by its interaction with the outflowing radio plasma; c) the evidence for an interaction is weaker in some radio galaxies. It is argued that the ionization of the ELG may be predominantly produced by the nuclear ultraviolet continuum and the kinematics of the gas due to the gravitational potential of the host galaxy, but it is not yet known whether there is a physical relationship between the ELG and the extended radio jets.

Type
Relation between Radio and Other Wavelenghts
Information
Symposium - International Astronomical Union , Volume 175: Extragalactic Radio Sources , 1996 , pp. 236 - 237
Copyright
Copyright © Kluwer 1996 

References

Baum, S.A., Heckman, T. (1989a) Extended Optical Line Emitting Gas in Powerful Radio Galaxies: Statistical Properties and Physical Conditions, ApJ , 336, pp. 681–701.Google Scholar
Baum, S.A., Heckman, T. (1989b) Extended Optical Line Emitting Gas in Powerful Radio Galaxies: What is the Radio Emission-Line Connection?, ApJ , 336, pp. 702–721.CrossRefGoogle Scholar
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Carrillo, R., Cruz-González, I., Guichard, J. (1995) in preparation.Google Scholar