[Previous] | [Session 6] | [Next]
S.D. Friedman, K.R. Sembach, J.C. Howk (Johns Hopkins University), B.D. Savage (University of Wisconsin), D.G. York (University of Chicago), G. Sonneborn (NASA Goddard Space Flight Center), FUSE Science Team
The Large and Small Magellanic Clouds are excellent laboratories for interstellar absorption line studies at far-ultraviolet wavelengths. The absorption can be viewed directly against the far-UV spectra of hot stars situated in the Clouds. In particular, the study of hot gas and its relationship with large-scale structures can be compared by observing such stars in the LMC, SMC, and Milky Way.
We report on FUSE observations of interstellar O VI in the direction of SK-67 05, an O9.7 Ib star in the western disk of the LMC. The data were obtained during the in-orbit checkout phase of the mission, prior to completion of instrument focus and alignment. We discuss the O VI content in the halo of the LMC and compare it with limits on column densities of other ions, such as C IV, from data obtained with IUE. The FUSE spectrum reveals a complex absorption pattern produced by atomic and molecular gas in the Milky Way halo and the LMC.
This work is supported by NASA contract NAS5-32985.
If you would like more information about this abstract, please follow the link to http://fuse.pha.jhu.edu. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.
The author(s) of this abstract have provided an email address for comments about the abstract: scott@pha.jhu.edu