The line of sight toward the SMC star Sk 108

Details The line of sight toward the SMC star Sk 108 The line of sight toward the SMC star Sk 108

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002phdt........12m&link_type=abstract

Thesis (PhD). THE UNIVERSITY OF CHICAGO, Source DAI-B 63/04, p. 1890, Oct 2002, 155 pages.

Computer Science

Scientific paper

I present the complete FUSE spectrum of the SMC Wolf-Rayet binary star Sk 108. The spectrum covers the 905 1186 Å wavelength range at a resolution of about 12,500 and a S/N of 25 50. I used detailed component information from higher resolution near-UV and optical spectra to model the far- UV lines. Although, both Galactic and SMC gas toward Sk 108 seem to be predominantly neutral, a significant fraction of the SMC gas is ionized. The Fe III/Fe II ratio as well as the column densities of O VI and P V are higher in the SMC than the Galaxy. The total H I column density is the same in the Galactic and SMC components. However, the column density of H2 is over an order of magnitude lower in the SMC. The excitation temperatures for the SMC are higher than the Galaxy, consistent with a stronger radiation field in the SMC. In addition to H2 measurements, I extend the abundance studies in this sight-line, to include Ar, P, N, O and S. The overall relative abundances agree with a lower dust-to-gas-metal ratio in the SMC than the Galaxy. The SMC clouds resemble typical Galactic halo abundance patterns, except for oxygen. Si, O and S are at roughly solar levels, relative to zinc, which might imply material enriched by massive stars or Type II SNe. N appears to be deficient in the SMC. In addition, I empirically determine oscillator strengths for a series of Fe II lines, using the pre-determined column densities for the Fe II components from the GHRS data. There are very few measurements of the elements seen here in QSOALS. More such measurements are needed at a range of redshifts. Similarly, abundances for MC targets are also at low numbers but the archival data of FUSE , in conjunction with high resolution ground- based spectra of the same targets, can be used to expand and more accurately determine depletions in the MC.

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