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Narrow Spectral Range Objective-Prism Technique Applied to A Search For Small Magellanic Cloud Members

Published online by Cambridge University Press:  12 April 2016

Marc Azzopardi
Marc Azzopardi*
Affiliation:
Dept. of Astronomy, University of Texas, Austin, TX 78712, USA

Extract

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The Magellanic Clouds are exceptional galaxies for the study of massive stars and other luminous objects, because they are close and seen in directions where the galactic interstellar extinction is relatively low. In addition the Small Magellanic Cloud (SMC) is of special interest because of the possible peculiar effects that its low metal abundance, compared to the Solar neighbourhood, may have on the evolution of its stellar population. Consequently, a search for the most luminous SMC members has been the subject of many studies. Among the different means used to detect SMC members, the wide field cameras equipped with objective prisms, Grisms or Grenses have played a prominent part. The method consists of selecting stellar objects showing high luminosity or typical spectral features. Such surveys have been especially successful in detecting SMC Ha emission-line objects (Henize, 1956; Lindsay, 1961), OB and blue supergiant stars (Sanduleak, 1968, 1969), planetary nebulae (Sanduleak et al., 1978; Sanduleak and Pesch, 1981) or carbon and late M-type stars (Blanco et al., 1980).

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 78: Astronomy with Schmidt-type telescopes , 1984 , pp. 351 - 354
Copyright
Copyright © Reidel 1984

References

Azzopardi, M.: 1981, Ph.D. thesis, Paul Sabatier University of Toulouse, No. 979, Vol. 1.Google Scholar
Azzopardi, M., Bijaoui, J., Marchal, J., Ounnas, Ch.: 1978, Astron. Astrophys. 65, 251.Google Scholar
Azzopardi, M., Breysacher, J.: 1979, Astron. Astrophys. 75, 120.Google Scholar
Azzopardi, M., Vigneau, J.: 1975, Astron. Astrophys. Suppl. 22, 285.Google Scholar
Azzopardi, M., Vigneau, J.: 1979, Astron. Astrophys. Suppl. 35, 355 Google Scholar
Azzopardi, M., Vigneau, J.: 1982, Astron. Astrophys. Suppl. 50, 291.Google Scholar
Blanco, V.M., McCarthy, M.F., Blanco, B.M.: 1980, Astrophys. J. 242, 938.Google Scholar
Breysacher, J., Lequeux, J.: 1983, The Messenger 33, 21.Google Scholar
Fehrenbach, Ch.: 1958, Handbuch der Physik, Vol. 50, p. 1.Google Scholar
Fehrenbach, Ch.: 1966, Eur. South. Obs. Bull. 1, 22.Google Scholar
Henize, K.G.: 1956, Astrophys. J. Suppl. 2, 315.Google Scholar
Lindsay, E.M.: 1961, Astron. J. 66, 169·Google Scholar
Martin, N., Rebeirot, E.: 1972, Astron. Astrophys. 21, 329.Google Scholar
Sanduleak, N.: 1968, Astron. J. 73, 246.Google Scholar
Sanduleak, N.: 1969, Astron. J. 74, 877.Google Scholar
Sanduleak, N., MacConnel, D. J., Davis Philip, A.G.: 1978, Publ. Astron. Soc Pacific 90, 621.Google Scholar
Sanduleak, N., Pesch, P.: 1981, Publ. Astron. Soc. Pacific 93, 431·CrossRefGoogle Scholar