0 FUSE Observations of O VI in High Velocity Clouds

We have used moderate-resolution (FWHM ≈ 25 km s −1) spectra of AGNs and QSOs observed by the Far Ultraviolet Spectroscopic Explorer to make the first definitive measurements of absorption by hot gas in high velocity clouds (HVCs) at large distances from the Galactic plane. Seven of the 11 sight lines studied exhibit high velocity (|V LSR | > 100 km s −1) O VI λ1031.93 absorption with log N(O VI) ≈ 13.79–14.62. High velocity O VI absorption is detected in the distant gas of H I HVC Complex C, the Mag-ellanic Stream, several HVCs believed to be in the Local Group, and the outer Galaxy. The fraction of O VI in HVCs along the seven sight lines containing high velocity O VI averages ∼30%, with a full range of ∼10–70%. The O VI detections imply that hot (T ∼ 3 × 10 5 K), collisionally-ionized gas is an important constituent of the HVCs since O VI is difficult to produce by photoionization unless the path lengths over which the absorption occurs are very large (>100 kpc). The association of O VI with H I HVCs in many cases suggests that the O VI may be produced at interfaces or mixing layers between the H I clouds and hot, low density gas in the Galactic corona or Local Group. Alternatively, the O VI may originate within cooling regions of hot gas clouds as they are accreted onto the Galaxy.