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J. Zsargo, K.R. Sembach (JHU), B.D. Savage (U. Wisconsin), C.G. Hoopes (JHU)
One of the major science objectives of the Far Ultraviolet Spectroscopic Explorer (FUSE) mission is to determine the extent and properties of hot gas in the interstellar medium by mapping the distribution of O~{\small VI} absorption in the Galactic halo. As part of this ongoing effort, we have obtained and analyzed FUSE spectra of 10 galactic O and B-type stars located at distances between ~00 and ~500 pc from the Galactic plane. The FUSE data cover the 905--1187 Å\ wavelength region and have S/N ratios of ~20-50 per 20 km~s-1 resolution element. Strong O~{\small VI} \lambda1031.93 absorption is detected toward all of these stars. The weaker member of the O~{\small VI} doublet at 1037.62 Å\ can be seen in the spectra of four stars, but strong H2 absorption is blended with the weaker O~{\small VI} line in the remaining cases. In this poster we present the kinematical structure of these O~{\small VI} lines, as well as the total O~{\small VI} column densities toward the target stars. We discuss our results in the the context of available information for other high ionization species (C~{\small IV} and N~{\small V}) and lower ionization stages (Si~{\small II} and Fe~{\small II}). We also compare the lower halo results with those found in a larger survey of O~{\small VI} along complete paths through the Galactic halo in the directions of quasars and active galactic nuclei. This work is based on data obtained for the Guaranteed Time Team by the NASA-CNES-CSA FUSE mission operated by the Johns Hopkins University. Financial support to U. S. participants has been provided by NASA contract NAS5-32985.