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Preprint typeset using L ATEX style emulateapj v. 04/03/99 FUSE OBSERVATIONS OF INTERSTELLAR GAS TOWARDS THE LMC STAR SK-67 05

By B. D. Savage, D. G. York, G. Sonneborn, A. Vidal-madjar and E. Wilkinson

Abstract

We report on measurements of interstellar O VI, H2, P II, Si II, Ar I, and Fe II absorption along the line of sight to Sk-67 05, a B0 Ia star in a diffuse H II region in the western edge of the Large Magellanic Cloud (LMC). We find log N(O VI) = 14.40 ± 0.04 in the Milky Way (MW) component and, 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 FUSE. In the LMC component, log N(O VI) = 13.89 ± 0.05, and N(C IV)/N(O VI) < 0.4 (3σ), since only an upper limit on N(C IV) is available. Along this sightline the LMC is rich in molecular hydrogen, log N(H2) = 19.50 ± 0.08; in the MW log N(H2) = 14.95 ± 0.08. A two-component fit for the excitation temperature of the molecular gas in the LMC gives T01 = 59 ± 5 K for J = 0, 1 and Tex = 800 ± 330 K for J = 3, 4, 5. For the MW, T01 = 99 +30 −20 K; no excitation temperature could be determined for the higher rotational states. The MW and LMC gas-phase [Fe/P] abundances are ∼ 0.6 and ∼ 0.7 dex lower, respectively, than solar system abundances. These values are similar to [Fe/Zn] measurements for the MW and LMC towards SN 1987A. Subject headings: galaxies: Milky Way, LMC – ISM:atoms – ultraviolet:ISM 1

Year: 2008
OAI identifier: oai:CiteSeerX.psu:10.1.1.317.5680
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