the SiC channels (which include the C III $\lambda$977 line). The redshift of each Magellanic Cloud is enough to separate the SNR C III emission (when present) from the back-scattered solar emission, but potential faint emission can still be lost in the higher background. For those objects with detected C III and/or O VI line emission, we have chosen to extract, plot, and measure the night-only fractions to avoid contamination problems when possible. (Two detected objects had no orbital night integration, however. See Table 2.)

The search for emission centered on the brightest transitions normally seen in the FUV – O VI $\lambda\lambda$1031.9138,1037.6154 and C III $\lambda$977.020. The O VI $\lambda$1032 line in the LiF1 channel was the primary feature searched for because the LiF1 channel has the highest effective area and the LWRS aperture position was known accurately. For most detected objects, the LiF2B channel also showed O VI emission, but at lower signal levels (due to the smaller effective area of this channel). O VI $\lambda$1038 was an important secondary indicator, although it is nearly always impacted severely by overlying absorption. Comparison with published grids of shock models (e.g., Hartigan, Raymond, & Hartmann 1987) indicate that strong C 