  We outline the results from a FUSE Team program designed to characterize OVI
absorption in the disk of the Milky Way. We find that OVI absorption occurs
throughout most of the Galactic plane, at least out to several kpc from the
Sun, and that it is distributed smoothly enough for the column density to
decline with height above the disk and with distance in the plane. However, the
OVI absorbing gas is clumpy, and moves at peculiar velocities relative to that
expected from Galactic rotation. We conclude that the observed absorption is
likely to be a direct indicator of the structures formed when violent,
dynamical processes heat the ISM, such as blowout from multiple supernovae
events.
