Abstract
We present measurements of the column densities of interstellar D I and O I made with the Far Ultraviolet Spectroscopic Explorer (FUSE) and of H I made with the International Ultraviolet Explorer (IUE) toward the sdOB star Feige 110 [(l,b) = (7409, - 5907); d = 179 pc; z = -154 pc]. Our determination of the D I column density made use of curve-of-growth fitting and profile fitting analyses, while our O I column density determination used only curve-of-growth techniques. The H I column density was estimated by fitting the damping wings of the interstellar Ly? profile. We find log N(D ) = 15.47 ? 0.06, log N(O ) = 16.73 ? 0.10, and log N(H ) = 20.14 (all errors 2 ?). This implies D/H = (2.14 ? 0.82) ? 10-5, D/O = ? 10-2, and O/H = (3.89 ? 1.67) ? 10-4. Taken with the FUSE results reported in companion papers and previous measurements of the local interstellar medium (LISM), this suggests the possibility of spatial variability in D/H for sight lines exceeding ~100 pc. This result may constrain models which characterize the mixing timescales and length scales of material in the LISM.
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