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A Plasmon Driven Bowshock Model for the Narrow Line Region of NGC 5929

Published online by Cambridge University Press:  12 April 2016

D. Taylor ,
J. E. Dyson ,
D. J. Axon  and
A. Pedlar
D. Taylor
Affiliation:
Department of Astronomy, University of Manchester, Manchester M13 9PL, U.K.
J. E. Dyson
Affiliation:
Department of Astronomy, University of Manchester, Manchester M13 9PL, U.K.
D. J. Axon
Affiliation:
Nuffield Radio Astronomy Observatories, Jodrell Bank, Macclesfield, Cheshire SK11 9DL, U.K.
A. Pedlar
Affiliation:
Nuffield Radio Astronomy Observatories, Jodrell Bank, Macclesfield, Cheshire SK11 9DL, U.K.

Extract

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Close links appear to exist between the optical narrow line region (NLR) in Seyfert galaxies and the nuclear non-thermal radio emission. Both occur on similar scales (~ 102 —103 pc), and correlations have been found between the 21 cm radio power and both the [OIII] λ5007Å luminosity and linewidth (de Bruyn & Wilson 1978; Whittle 1985). Approximate balance appears to exist between the thermal pressure of the NLR gas and the relativistic and magnetic pressure of the radio components (de Bruyn & Wilson 1978; Unger et al. 1985; Pedlar, Dyson & Unger 1985). There are also several examples of a direct spatial association between the optical and radio components, for example Mkn 78 (Pedlar et al. 1988).

Type
V. The Extragalactic ISM
Information
International Astronomical Union Colloquium , Volume 120: Structure and Dynamics of the Interstellar Medium , 1989 , pp. 364 - 368
Copyright
Copyright © Springer-Verlag 1989

References

De Bruyn, A. J. & Wilson, A. S., 1978. Astron. Astrophys., 64, 433.Google Scholar
Falle, S. A. E. G., 1975. Astron. Astrophys., 42, 323.Google Scholar
Ferland, G. J. & Osterbrock, D. E., 1986. Astrophys. J., 300, 658.CrossRefGoogle Scholar
Pedlar, A., Dyson, J. E. & Unger, S. W., 1985. Mon. Not. R. astr. Soc., 214, 463.CrossRefGoogle Scholar
Pedlar, A., Meaburn, J., Axon, D. J., Unger, S. W., Guerrine, N., Whittle, M., Meurs, P. & Ward, M., 1989. Mon. Not. R. astr. Soc., 238, 863.CrossRefGoogle Scholar
Ulvestad, J. S. & Wilson, A. S., 1984. Astrophys. J., 285, 439.CrossRefGoogle Scholar
Unger, S. W., Pedlar, A., Booler, R. V. & Harrison, B. A., 1985. Mon. Not. R. astr. Soc., 219, 387.CrossRefGoogle Scholar
Whittle, M., 1985. Mon. Not. R. astr. Soc., 213, 33.CrossRefGoogle Scholar
Whittle, M., Haniff, C. F., Ward, M. J., Meurs, E. J. A., Pedlar, A., Unger, S. W., Axon, D. J. & Harrison, B. A., 1986. Mon. Not. R. astr. Soc., 222, 189.CrossRefGoogle Scholar
Wilson, A. S. & Ulvestad, J. S., 1983. Astrophys. J., 275, 8.CrossRefGoogle Scholar