The deuterium, oxygen, and nitrogen abundance toward LSE 44

We present measurements of the column densities of interstellar D I, O I, NI, and H-2 made with the Far Ultraviolet Spectroscopic Explorer ( FUSE) and of H I made with the International Ultraviolet Explorer (IUE) toward the sdO star LSE 44 [(l, b) (313 degrees.37, +13 degrees.49); d = 554 +/- 66 pc; z = +129 +/- 15 pc]. This target is among the seven most distant Galactic sight lines for which these abundance ratios have been measured. The H I column density was estimated by fitting the damping wings of interstellar Ly alpha. The column densities of the remaining species were determined with profile fitting analyses and supplemented with curve-of-growth analyses for O I and H-2. We find logN(D I) 15:87 +/- 0: 08, log N(O I) 17: 57(-0.15)(+0.21), logN(N I) 16: 43 +/- 0: 14, and log N( H I) 20:52(-0: 36)(+0.20) (all errors 2 sigma). This implies that D/ H (2: 24(-1.32)(+1.39)); 10(-5), D/O (1: 99(-0.67)(+1.30)); 10(-2), D/N (2: 75(-0).(+1.19)(89)); 10(-1), and O/H (1.13(-0.71)(+0.96)); 10 (-3). Of the most distant Galactic sight lines for which the deuterium abundance has been measured, LSE 44 is one of the few with D/H higher than the Local Bubble value, but D/O toward all these targets is below the Local Bubble value and more uniform than the D/H distribution.