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| Paper: |
High-velocity O VI In and Near the Milky Way |
| Volume: |
331, Extra-Planar Gas |
| Page: |
11 |
| Authors: |
Wakker, B.P.; Savage, B.D.; Sembach, K.R.; Richter, P.; Fox, A.J. |
| Abstract: |
The Far Ultraviolet Spectroscopic Explorer (FUSE) has observed over three hundred fifty sight-lines to extragalactic targets. About one hundred fifty of these are of sufficient quality to measure O VI absorption in and near the Milky Way. High-velocity O VI absorption is detected in about 80% of the sight-lines, with the detection rate going up for sight-lines with higher signal-to-noise ratios. O VI is almost always seen in directions with previously known H I HVCs, including HVCs complex C, complex A, complex WD, the Magellanic Stream, and the Outer Arm. Studies of several sight-lines through complex C suggest that the O VI absorption is produced in conductive interfaces between the cool HVC and a hotter surrounding medium, most likely a corona around the Milky Way. The O VI detections associated with the Magellanic Stream imply that this hot corona has a radius of at least 50 kpc. About half of the detections of high-velocity O VI are in directions where no high-velocity H I was previously known. Some of these are probably associated with the Magellanic Stream, others may represent Local Group gas. Still others often show up as a distinct wing on the low-velocity absorption; these may either represent an outflow from the Milky Way associated with the Galactic Fountain, they may be extragalactic HVCs, or they may be tracing a wind from the Galactic Center. Distance limits to the high-velocity O VI are scarce, but at least one of the clouds appear to be more distant than 4 kpc. |
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