Far Ultraviolet Spectroscopic Explorer observations of interstellar gas toward the large magellanic cloud star Sk-67 degrees 05

We report on measurements of interstellar O VI, H-2, P II, Si II, Ar I, and Fe II absorption along the line of sight to Sk -67 degrees 05, a B0 Ia sta r in a diffuse H II region in the western edge of the Large Magellanic Clou d (LMC). We find log N(O VI) = 14.40 +/- 0.04 in the Milky Way component an d, using the C Iv column density from previous IUE observations, N(C IV)/N( O VI) = 1.00 +/- 0.16, a value similar to other halo measurements made with the Far Ultraviolet Spectroscopic Explorer. In the LMC component, log N(O VI) = 13.89 +/- 0.05 and N(C IV)/N(O VI) < 0.4 (3 a), since only an upper l imit on N(C Iv) is available. Along this sight line, the LMC is rich in mol ecular hydrogen [log N(H-2) = 19.50 +/- 0.08]; in the Milky Way, log N(H-2) = 14.95 +/- 0.08. A two-component fit for the excitation temperature of th e molecular gas in the LMC gives T-01 = 59 +/- 5 K for J = 0, 1 and T-ex = 800 +/- 330 K for J = 3, 4, 5. For the Milky Way, T-01 = 99(-20)(+30) K; no excitation temperature could be determined for the higher rotational state s. The Milky Way and LMC gas-phase [Fe/P] abundances are similar to 0.6 and similar to 0.7 dex lower, respectively, than solar system abundances. Thes e values are similar to [Fe/Zn] measurements for the Milky Way and LMC towa rd SN 1987 A.