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Far Ultraviolet Spectroscopic Explorer Observations of Interstellar Gas toward the Large Magellanic Cloud Star Sk –67°05

, , , , , , , , , , , and

Published 19 July 2000 • © 2000. The American Astronomical Society. All rights reserved. Printed in U.S.A.
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Author affiliations

1 Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218

2 Department of Astronomy, University of Wisconsin, Madison, WI 53706

3 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637

4 Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771

5 Institut d'Astrophysique de Paris, Centre National de la Recherche Scientifique, 98 bis Boulevard Arago, F-75014 Paris, France

6 Center for Astrophysics and Space Astronomy, University of Colorado, Campus Box 389, Boulder, CO 80309

Dates

Received 24 March 2000
Accepted 8 June 2000
Published

Citation

S. D. Friedman et al 2000 ApJ 538 L39

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DOI

https://doi.org/10.1086/312800

Keywords

galaxies: individual (Large Magellanic Cloud) ; ISM: atoms; ultraviolet: ISM

Journal RSS feed

1538-4357/538/1/L39

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 img1.gif) = 14.40 ± 0.04 in the Milky Way component and, using the C IV column density from previous IUE observations, N(C img2.gif)/N(O img1.gif) = 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 img1.gif) = 13.89 ± 0.05 and N(C img2.gif)/N(O img1.gif) < 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 = 99img3.gif 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.

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