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Co-ordinated Optical and Radio Observations of Symbiotic Stars

Published online by Cambridge University Press:  12 April 2016

R. J. Ivison ,
M. F. Bode ,
J. Meaburn ,
R. J. Davis ,
R. F. Nelson  and
R. E. Spencer
R. J. Ivison
Affiliation:
School of Physics & Astronomy, Lancashire Polytechnic, Corporation St., Preston, PR1 2TQ, U. K.
M. F. Bode
Affiliation:
School of Physics & Astronomy, Lancashire Polytechnic, Corporation St., Preston, PR1 2TQ, U. K.
J. Meaburn
Affiliation:
Department of Astronomy, University of Manchester, Manchester, M13 9PL, U. K.
R. J. Davis
Affiliation:
Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire, SK11 9DL, U. K.
R. F. Nelson
Affiliation:
Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire, SK11 9DL, U. K.
R. E. Spencer
Affiliation:
Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire, SK11 9DL, U. K.

Abstract

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We present preliminary results from absolutely flux-calibrated optical spectroscopy, together with 5 GHz radio flux measures of 17 symbiotic stars. The data were obtained quasi-simultaneously using the Manchester Echelle Spectrograph on the Isaac Newton Telescope, La Palma between 1988 September 20 and 24, and the Broad Band Interferometer at Jodrell Bank during 1988 October. This represents the largest sample of these stars observed in this way to date. Distances are calculated using visual extinctions and are compared with other quoted values. In general, the agreement is surprisingly good. Plots of individual line luminosities vs. radio luminosity indicate that the D-type (dusty) symbiotics (both also proto-planetary nebulae) have far higher radio luminosities than S-types (stellar) for comparable recombination and forbidden line luminosities. This may however be due to underestimation of optical line luminosities for the D-types as the circumstellar extinction contribution is uncertain. The single D’-type (cool dust, yellow secondary) lies at the low luminosity end of the S-type region. ‘Very slow novae’ in our sample lie in both groups.

Type
4. Related Objects
Information
International Astronomical Union Colloquium , Volume 122: Physics of Classical Novae , 1990 , pp. 442 - 443
Copyright
Copyright © Springer-Verlag 1990

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