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B. Otte, W. V. Dixon, R. Sankrit (Johns Hopkins Univ.)
We present long integration (95 ksec) data of Galactic OVI emission taken with the {\em Far Ultraviolet Spectroscopic Explorer (FUSE)} at l=95.5\circ and b=36\circ. This sight line points towards a region of stronger-than-average soft X-ray emission and lies above a part of the disk where the warp of the outer Galaxy extends to high Galactic latitudes. The interstellar medium in galaxies consists of several phases, with the hottest phase reaching temperatures of a few million degrees. This hot ionized medium is observed in X-ray emission. The OVI emission observed in the far ultraviolet wavelength regime is thought to be a tracer of gas that has been heated up by shocks from supernova explosions and is now cooling down, because such high ionization stages cannot be achieved by photoionization from hot stars. We measure the observed OVI emission and estimate the physical parameters of the gas along our line of sight.
This research is supported by NASA contract NAS5-32985 to the Johns Hopkins University.
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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.