Deuterium abundance toward g 191-b 2 b : results from the fuse mission 1

High-resolution spectra of the hot white dwarf G191-B2B, covering the wavelength region 905–1187 Å, were obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE). These data were used in conjunction with existing high-resolution Hubble Space Telescope Space Telescope Imaging Spectrograph (STIS) observations to evaluate the total H i, D i, O i, and N i column densities along the line of sight. Previous determinations of N(D i) based upon GHRS and STIS observations were controversial as a result of the saturated strength of the D i Ly line. In the present analysis the column density of D i has been measured using only the unsaturated Ly and Ly lines observed by FUSE. A careful inspection of possible systematic uncertainties tied to the modeling of the stellar continuum or to the uncertainties in the FUSE instrumental characteristics has been performed. The column densities derived are logNðD iÞ 1⁄4 13:40 0:07, logNðO iÞ 1⁄4 14:86 0:07, and logNðN iÞ 1⁄4 13:87 0:07, quoted with 2 uncertainties. The measurement of the H i column density by profile fitting of the Ly line has been found to be uncertain. If additional weak, hot interstellar components are added to the three detected clouds along the line of sight, the H i column density can be reduced quite significantly, even though the signal-to-noise ratio and spectral resolution at Ly are excellent. The new estimate of N(H i) toward G191-B2B reads logNðH iÞ 1⁄4 18:18 0:18 (2 ), so that the average D/H ratio on the line of sight is D=H 1⁄4 1:66þ0:9 0:6 10 5 (2 ). Subject headings: ISM: abundances — ISM: clouds — stars: individual (G191-B2B) — ultraviolet: ISM