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[ITAL]Far Ultraviolet Spectroscopic Explorer[/ITAL] Observations of Interstellar Gas toward the Large Magellanic Cloud Star S[CLC]k[/CLC] −67°05

2000; IOP Publishing; Volume: 538; Issue: 1 Linguagem: Inglês

10.1086/312800

1538-4357

S. D. Friedman, J. Christopher Howk, B. G. Andersson, Kenneth R. Sembach, Thomas B. Ake, Katherine C. Roth, David J. Sahnow, Blair D. Savage, Donald G. York, G. Sonneborn, A. Vidal‐Madjar, E. Wilkinson,

Gamma-ray bursts and supernovae

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 ) = 14.40 ± 0.04 in the Milky Way component and, using the C IV column density from previous IUE observations, N(C )/N(O ) = 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 ) = 13.89 ± 0.05 and N(C )/N(O ) < 0.4 (3 σ), since only an upper limit on N(C IV) is available. Along this sight line, the LMC is rich in molecular hydrogen [log N(H2) = 19.50 ± 0.08]; in the Milky Way, 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 Milky Way, T01 = 99 K; no excitation temperature could be determined for the higher rotational states. The Milky Way 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 Milky Way and LMC toward SN 1987A.