The Small Magellanic Cloud. I - A study of the structure revealed by the supergiants

Details The Small Magellanic Cloud. I - A study of the structure revealed by the supergiants The Small Magellanic Cloud. I - A study of the structure revealed by the supergiants

Apr 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....56..151a&link_type=abstract

Astronomy and Astrophysics, vol. 56, no. 1-2, Apr. 1977, p. 151-161.

Astronomy and Astrophysics

Astrophysics

57

Galactic Structure, Magellanic Clouds, Star Distribution, Supergiant Stars, H Ii Regions, Interstellar Extinction, Star Clusters, Star Formation Rate, Stellar Evolution, Stellar Spectra

Scientific paper

The structure of the Small Magellanic Cloud (SMC) is studied on the basis of the distribution of 465 supergiants belonging to that galaxy. The distribution of the supergiants according to spectral type is shown to be 64 per cent O9-B2, 11 per cent B3-B6, 20 per cent B7-A9, and 5 per cent F-G. It is found that these stars are concentrated in five accumulation zones located in the southwest part of the bar, at the northwest border of the bar, in the northeast part of the bar, and (two zones) in the wing. The location of emission-line stars, red and blue clusters, and H II regions relative to the supergiant accumulation zones is investigated, and a correlation between O-B2 supergiants and neutral hydrogen is determined which indicates a star formation rate similar to that for other galaxies. Analysis of interstellar reddening shows that the mean absorption in the SMC is low and that the gas/dust ratio is 15 times higher than in the Galaxy.

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