  We used the FUSE (Far Ultraviolet Spectroscopic Explorer) satellite to
observe OVI emission along two sightlines towards the edge of the interaction
zone (IZ) between the Loop I superbubble and the Local Bubble. One sightline
was chosen because material in the interaction zone blocks distant X-ray
emission, and should thus do the same for non-local OVI emission. We measured
an OVI intensity of I_shadowed = 2750 +- 550 L.U. along this `Shadowed'
sightline, and I_unshadowed = 10800 +- 1200 L.U. along the other sightline.
Given these results, very little (< 800 L.U.) of the emission arises from the
near side of the interaction zone, which likely has an HI column density of
about 4e+20 cm-2 along the `Shadowed' sightline. The OVI emission arising
within Loop I (~1e+4 L.U.) is probably associated with gas of n_e ~ 0.1 cm-3
and an emitting pathlength of ~1.2 pc, suggesting it arises at interfaces
rather than from gas filling Loop I. In contrast, the CIII emission is similar
along both sightlines, indicating that much of the emission likely arises on
the near side of the interaction zone.
