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Observations obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE)have been used to determine the column densities of D I, O I, and N I alongseven sight lines that probe the local interstellar medium (LISM) at distancesfrom 37 pc to 179 pc. Five of the sight lines are within the Local Bubble andtwo penetrate the surrounding H I wall. Reliable values of N(H I) weredetermined for five of the sight lines from HST data, IUE data, and publishedEUVE measurements. The weighted mean of D I/H I for these five sight lines is(1.52 +/- 0.08) x10-5 (1 sigma uncertainty in the mean). It is likely that theD I/H I ratio in the Local Bubble has a single value. The D I/O I ratio for thefive sight lines within the Local Bubble is (3.76 +/- 0.20) x10-2. It is likelythat the O I column densities can serve as a proxy for H I in the Local Bubble.The weighted mean for O I/H I for the seven FUSE sight lines is (3.03 +/-0.21)x10-4, comparable to the weighted mean (3.43 +/- 0.15) x10-4 reported for 13sight lines probing larger distances and higher column densities (Meyer et al.1998, Meyer 2001). The FUSE weighted mean of N I/H I for the five sight linesis half that reported by Meyer et al. (1997) for seven sight lines with largerdistances and higher column densities. This result combined with thevariability of O I/N I (six sight lines) indicates that at the low columndensities found in the LISM, nitrogen ionization balance is important. Thus,unlike O I, N I cannot be used as a proxy for H I or as a metallicity indicatorin the LISM.  Subject Headings: cosmology: observations- ISM: abundances- ISM: evolution -Galaxy:abundances-Ultraviolet:ISMComment: 36 pages, 5 figures, 4 table

Abundances of Deuterium, Nitrogen, and Oxygen in the Local Interstellar Medium: Overview of First Results from the FUSE Mission