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Strömgren photometry of supergiants in the Magellanic Clouds

Published online by Cambridge University Press:  25 April 2016

S. C. Russell ,
M. S. Bessell  and
M. A. Dopita
S. C. Russell
Affiliation:
Mount Stromlo and Siding Spring Observatories, The Australian National University
M. S. Bessell
Affiliation:
Mount Stromlo and Siding Spring Observatories, The Australian National University
M. A. Dopita
Affiliation:
Mount Stromlo and Siding Spring Observatories, The Australian National University
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Abstract

This is a preliminary report on the first Strömgren–Hβ photometric survey of yellow supergiants in the Magellanic Clouds. Less luminous supergiants have been chosen in preference for this program in order to facilitate calculation of their physical parameters. This will not only provide a basis for future detailed spectral analysis of these stars, but will allow a better calibration of the colours derived from model atmospheres for this type of star. The colours of these stars are more affected by changes in metallicity than the hotter stars more frequently studied, and since they are also young, they reflect the metallicity of their local InterStellar Medium (ISM). If indeed the Strömgren abundance index m1 can be calibrated successfully for these stars, then their observation in any galaxy will provide the metallicity of that particular ISM. Our results show that it is important for future colours to be calculated over the range of turbulent velocities important for supergiants.

Type
Stellar
Information
Publications of the Astronomical Society of Australia , Volume 7 , Issue 1 , 1987 , pp. 65 - 68
Copyright
Copyright © Astronomical Society of Australia 1987

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References

Ardeberg, A., Brunet, J.-P., Maurice, E. and Prévot, L., 1972, Astron. Astrophys. Suppl. Ser., 6, 249.Google Scholar
Azzopardi, M. and Vigneau, J., 1975, Astron. Astrophys. Suppl. Ser., 22, 285.Google Scholar
Bessell, M. S. and Russell, S. C., 1987, in preparation.Google Scholar
Caldwell, J. A. R. and Coulson, I. M., 1985, Mon. Not. R. Astron. Soc., 212, 879.Google Scholar
Fehrenbach, Ch. and Duflot, M., 1970, Astron. Astrophys. Special Suppl. Ser., 1.Google Scholar
Hauck, B. and Mermilliod, M., 1975, Astron. Astrophys., 22, 235.Google Scholar
Kurucz, R. L., 1979, Astrophys. J. Suppl. Ser., 40, 1.Google Scholar
McNamara, D. H. and Feltz, K. A. Jr., 1980, Publ. Astron. Soc. Pac., 92, 587.Google Scholar
Olsen, E. H., 1983, Astron. Astrophys. Suppl. Ser., 54, 55.Google Scholar
Osmer, P. S., 1973, Astrophys. J., 181, 327.Google Scholar
Philip, A. G. D. and Relyea, L. J., 1979, Astron. J., 84, 1743.Google Scholar
Relyea, L. J. and Kurucz, R. L., 1978, Astrophys. J. Suppl. Ser., 37, 45.Google Scholar
Russell, S. C., Bessell, M. S. and Dopita, M. A., 1987, in preparation.Google Scholar
Schmidt, E. G., 1979, Astron. J., 84, 1739.Google Scholar
Shobbrook, R. R. and Visvanathan, N., 1987, Mon. Not. R. Astron. Soc., 225, 947.Google Scholar