Emission via the O VI doublet at 1031.93 and 1037.62 Å is the primary cooling mechanism for interstellar gas at temperatures between 10⁵ and 10⁶ K. As such, it traces regions where hot gas cools quiescently, interface regions where hot and cool gas meet and mingle, and high-velocity shocks. Over its eight-year mission, the Far Ultraviolet Spectroscopic Explorer (FUSE) was used to observe O VI in both emission and absorption. In this talk, I will present a brief history of the hot component of the interstellar medium (ISM) and the various physical processes responsible for its creation, evolution, and morphology. I will review the results of recent O VI absorption- line studies of the Galactic disk and halo. Finally, I will present the latest results of our survey of diffuse O VI emission from the ISM.

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