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Subarcsecond-Scale Optical and Radio Structure Correlations in Seyfert Galaxies

Published online by Cambridge University Press:  19 July 2016

R.W. Pogge  and
M.M. Derobertis
R.W. Pogge
Affiliation:
Department of Astronomy, The Ohio State University, Columbus, Ohio, USA
M.M. Derobertis
Affiliation:
Department of Physics & Astronomy, York University, North York, Ontario, Canada

Extract

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An unanswered question in the study of Seyferts is the nature of the relationship between the extended radio-continuum and optical emission-line gas. Detailed comparison is difficult as most Seyferts have radio structure on sub-arcsecond scales, while most optical imaging is on 1–2″ scales. Despite this, some basic features have emerged. Extended radio and optical emission regions are generally aligned in projection, but the overall optical emission extends to much greater galactocentric radii. Pedlar et al. (1989) and Whittle et al. (1986) have reported a tendency for optical emission knots to lie behind the radio lobes, interpreted in terms of the “cooling length” of gas heated by a radiative bowshock driven into the ISM by a jet. In NGC 1068 (Cecil et al. 1990) and M51 (Cecil 1988), however, ambient gas appears to be piling up ahead of a radio lobe at the terminus of the radio jet.

Type
Poster Contributions: Line Studies
Information
Symposium - International Astronomical Union , Volume 159: Multi-Wavelength Continuum Emission of AGN , 1994 , pp. 455
Copyright
Copyright © Kluwer 1994 

References

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