Computer Science
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6567b&link_type=abstract
HST Proposal ID #6567
Computer Science
Hst Proposal Id #6567 Hot Stars
Scientific paper
In cycle 1 and cycle 4 we obtained FOS spectra of individual early type stars in M31 and M33. Combined with ground based data, the UV spectra were used to study stellar atmospheres and winds and compare wind velocities, mass loss rates, and abundances with similar galactic and LMC stars. We analysed the data by modeling line profiles with different methods, and made direct comparison between spectra of similar stars in different galaxies. Detailed study of hot star populations in galaxies outside the Milky Way provides a very important test of theories of stellar winds, star formation and evolution. Extinction properties of the ISM in the UV are also derived from the continuum distribution. We propose to extend these comparisons to the Local Group irregular galaxy NGC6822. Here the foreground extinction poses more severe limitations than in M31 and M33, but we have found 5 targets, from extensive optical work {Massey et al.1995}, that are accessible to FOS/GHRS and will provide a small but highly valuable exploratory sample. Our ground based spectroscopy indicates that the metal lines in NGC6822 B-supergiants are significantly weaker than in SMC stars of similar spectral type and luminosity, which is inconsistent with the considerably higher than SMC-like metallicity indicated by HII region studies. HST spectroscopy in the UV provides valuable information about the metallicity.
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