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Discovery of a Reflection Dust Envelope Around IRC+10216

Published online by Cambridge University Press:  12 April 2016

M. Tamura ,
T. Hasegawa ,
N. Ukita ,
I. Gatley ,
I. S. McLean ,
M. G. Burton ,
J. T. Rayner  and
M. J. McCaughrean
M. Tamura
Affiliation:
Department of Physics, Kyoto University, Japan.
T. Hasegawa
Affiliation:
Nobeyama Radio Observatory, Tokyo Astronomical Observatory, University of Tokyo, Japan.
N. Ukita
Affiliation:
Nobeyama Radio Observatory, Tokyo Astronomical Observatory, University of Tokyo, Japan.
I. Gatley
Affiliation:
United Kingdom Infrared Telescope Unit, Hawaii.
I. S. McLean
Affiliation:
United Kingdom Infrared Telescope Unit, Hawaii.
M. G. Burton
Affiliation:
United Kingdom Infrared Telescope Unit, Hawaii.
J. T. Rayner
Affiliation:
Department of Astronomy, University of Edinburgh, U.K.
M. J. McCaughrean
Affiliation:
Department of Astronomy, University of Edinburgh, U.K.

Extract

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Infared polarimetric and photometric mapping observations at K(2.2 μm) and H(1.65 μm) have revealed an extended dust envelope around the late-type star IRC+10216. The observations were made on the 3.8-m United Kingdom Infrared Telescope on Mauna Kea, Hawaii, in 1985 December and 1987 January and February. The polarization observations were made by emplying the Kyoto polarimeter (Sato et al. 1987). Great care was taken to check the contamination by stray light in the telescope and instruments as the source on peak was extremely bright (K~0 mag). From the observations of normal stars, we found that the polarized intensity (degree of polarization times the intensity) was a good measure of the envelope, free from contamination by stray light, although the intensity and the degree of polarization suffered from the contamination separately.

Type
Part II. Mass-Losing Stars in Different Stages of Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 181 - 182
Copyright
Copyright © Springer-Verlag 1988

References

Bieging, J.H., Chapman, B., and Welch, W.J. 1984, Ap. J., 285, 656 Google Scholar
Sato, S. et al. 1987, M.N.R.A.S., in press.Google Scholar
Wannier, P.G., Leighton, R.B., Knapp, G.R., Redman, R.O., Phillips, T.G., and Huggins, P.J. 1979, Ap. J., 230, 149 Google Scholar
Wilson, W.J., Schwartz, P.R., and Epstein, E.E. 1973, Ap. J., 183, 871 Google Scholar
Wootten, A., Lichten, S.M., Sahai, R., and Wannier, P.G. 1982, Ap. J., 257, 151.CrossRefGoogle Scholar