We present measurements of the column densities of interstellar D I , O I , N I , 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 \fdg 37 , +13 \fdg 49 ) ; d = 554 \pm 66 pc ; z = +129 \pm 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 log N ( D I ) = 15.87 \pm 0.08 , log N ( O I ) = 17.57 ^ { +0.21 } _ { -0.15 } , log N ( N I ) = 16.43 \pm 0.14 , and log N ( H I ) = 20.52 ^ { +0.20 } _ { -0.36 } ( all errors 2 \sigma ) . This implies D/H = ( 2.24 ^ { +1.39 } _ { -1.32 } ) \times 10 ^ { -5 } , D/O = ( 1.99 ^ { +1.30 } _ { -0.67 } ) \times 10 ^ { -2 } , D/N = ( 2.75 ^ { +1.19 } _ { -0.89 } ) \times 10 ^ { -1 } , and O/H = ( 1.13 ^ { +0.96 } _ { -0.71 } ) \times 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 .