Other
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...20111311p&link_type=abstract
American Astronomical Society, 201st AAS Meeting, #113.11; Bulletin of the American Astronomical Society, Vol. 34, p.1285
Other
Scientific paper
We present initial results from an abundance study of AV 304, a sharp-lined B0.5V star in the Small Magellanic Cloud, using recently-acquired spectroscopic data from the Far Ultraviolet Spectroscopic Explorer (FUSE) and the Kurucz LTE model atmosphere/spectrum synthesis codes ATLAS9/SYNTHE. Emphasis is on the abundances of the Fe group elements that do not produce measurable lines in the optical spectral region. A model of Teff = 26,500 K, log g = 4.0, and [M/H] = -0.5 was adopted based upon a least squares fit to IUE LORES data and the UBV magnitudes for the star. Other input parameters used included Vturb = 1 km s-1 (from the continuum fit), v sin i = 20 km s-1, and an instrumental broadening parameter of 20,000 corresponding to the spectral resolution of the FUSE LiF channels. A mean Fe abundance, [Fe/H]sun, of -0.70+/-0.3 was obtained from Fe 3 multiplets UV1 (1122--1132 Å) and UV39 (1142--1144 Å). This agrees well with the value of -0.61+/-0.30 found from 65 lines of Fe 3 in the 1900 Å, region observed with HST/STIS (Peters & Grigsby 2003, submitted) and also abundances determined from lines in the ISM and A supergiants. The abundance of V from V 3 UV2 (1148--1154 Å) appears to be close to the solar value, but more study is warranted. On the other hand, upper limits on the abundances of Cr and Mn from several Cr 3 and Mn 3 lines in the 1100--1160 Å, region are 1.0 dex below the solar values. This supports the results from the Peters/Grigsby analysis of HST/STIS spectra in which abundances of -1.00 dex were found for both elements. GJP appreciates support from NASA grant NAG5-12239.
Adelman Saul J.
Peters Geraldine Joan
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