Spectral types of red supergiants in Magellanic Cloud clusters

Details Spectral types of red supergiants in Magellanic Cloud clusters Spectral types of red supergiants in Magellanic Cloud clusters

Mar 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.186..831f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 186, Mar. 1979, p. 831-836.

Astronomy and Astrophysics

Astronomy

13

Late Stars, Magellanic Clouds, Red Giant Stars, Star Clusters, Stellar Spectra, Supergiant Stars, Abundance, Astronomical Spectroscopy, Cepheid Variables, Stellar Luminosity

Scientific paper

Spectra (30 Å/mm) have been obtained of eight red supergiants in the young cluster NGC 330 (SMC) and four in NGC 2004 (LMC). In NGC 330 the spectral types (˜G5 Ib) are earlier than for galactic supergiants of the same colour ((B-V) = 1.3-1.6). In NGC 2004 the stars are of later type (˜KO Ib) than in NGC 330 at these colours. The NGC 330 stars show some evidence for a metal deficiency (CN weak, H strong). VV Cep-like systems have been found in each of three young clusters so far studied (NGC 330, 2004, 2100) indicating a relatively high frequency for such systems.

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