  We have used the Far Ultraviolet Spectroscopic Explorer to search for OVI
1031.926, 1037.617 A emission in the halos of the edge-on spiral galaxies
NGC4631 and NGC891. In NGC4631, we detected OVI in emission toward a soft X-ray
bubble above a region containing numerous Halpha arcs and filaments. The
line-of-sight component of the motion of the OVI gas appears to match the
underlying disk rotation. The observed OVI luminosities can account for 0.2-2%
of the total energy input from supernovae (assuming a full OVI emitting halo)
and yield mass flux cooling rates between 0.48 and 2.8 M_sun/yr depending on
the model used in the derivations. Based on these findings, we believe it is
likely that we are seeing cooling, galactic fountain gas. No emission was
detected from the halo of NGC891, a galaxy in a direction with considerably
high foreground Galactic extinction.
