Interstellar Deuterium, Nitrogen and Oxygen Abundances Toward BD+28(deg) 4211: Results from the Far Ultraviolet Spectroscopic Explorer

High resolution far-ultraviolet spectra of the O-type subdwarf BD+28(deg)4211 were obtained with the Far Ultraviolet Spectroscopic Explorer to measure the interstellar deuterium, nitrogen, and oxygen abundances in this direction. The interstellar D(I) transitions are analyzed down to Ly(ioat) at 920.7 A. The star was observed several times at different target offsets in the direction of spectral dispersion. The aligned and coedited spectra have high signal-to-noise ratios (S/N=50-100). D(I), N(I), and O(I) transitions were analyzed with curve-of-growth and profile fitting techniques. A model of interstellar molecular hydrogen on the line of sight was derived from H(II) lines in the FUSE spectra and used to help analyze some features where blending with H(II) was significant. The H(I) column density was determined from high resolution HST/STIS spectra of Ly(alpha) to be log N(H(I))= 19.846+/-0.035(2sigma), which is higher than is typical for sight lines in the local ISM studied for D/H. We found that D/H=(1.39+/-0.21)x 10(exp -5)(2sigma) and O/H=(2.37+/-0.55)x10(exp -4)(2sigma). O/H toward BD+28(deg)4211 appears to be significantly below the mean O/H ratio for the ISM and the Local Bubble.