Observations of the UV-Bright Star BS in 47 Tucanae with the Hopkins Ultraviolet Telescope

Details Observations of the UV-Bright Star BS in 47 Tucanae with the Hopkins Ultraviolet Telescope Observations of the UV-Bright Star BS in 47 Tucanae with the Hopkins Ultraviolet Telescope

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...186.2215d&link_type=abstract

American Astronomical Society, 186th AAS Meeting, #22.15; Bulletin of the American Astronomical Society, Vol. 27, p.843

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Scientific paper

The UV-bright star BS in the globular cluster 47 Tuc was observed with the Hopkins Ultraviolet Telescope (HUT) during the Astro-2 space shuttle mission in 1995 March. The resulting spectrum extends from the interstellar cutoff at 912 Angstroms to 1850 Angstroms with a resolution of ~ 3 Angstroms. It shows numerous absorption features, but no significant emission features other than terrestrial airglow lines. Detailed fitting of Kurucz stellar atmosphere models using a chi (2) minimization technique indicates Teff = 11,000 K, log g = 2.5, and log Z/Z_&sun; = -1.0. The Kurucz model which best fits the observed spectrum overpredicts the flux in the Lyman gamma to Lyman beta region by nearly a factor of three, suggesting that opacity effects not included in the models are important even at this relatively low temperature. Assuming a distance of 4.6 +/- 1.0 kpc, we estimate the stellar luminosity to be log L/L_&sun; = 3.1 +/- 0.2. These atmospheric parameters place the star on the Schonberner post-AGB evolutionary tracks. The Hopkins Ultraviolet Telescope Project is supported by NASA contract NAS 5-27000 to The Johns Hopkins University.

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