+165 $\VEL$ for SMC). The longest tick marks indicate the expected positions of C III and O VI lines. Of course, the same transitions that we expect from the SNRs in emission are strong resonance lines that can also be in absorption from the intervening ISM at both galactic and MC velocities.

Many objects detected in our survey show both O VI and C III emission at detectable levels. Interestingly, some objects show O VI but no C III (e.g., SNR 0509-687), but there is only one detection in C III-only (SNR 0527-658), and this detection is marginal. The presence of O VI emission in most of the detected objects indicates that each of them has some shocks with velocities in excess of 160 $\VEL$. In SNR 0527-658, at least at the observed location, such shocks are apparently absent. Additional observations at other locations within SNR 0527-658 would be needed to understand whether the absence of O VI is intrinsic to the object or due to the clumpiness of the O VI spatial distribution.

We have measured the observed line widths, approximate centroid velocities, and integrated total line fluxes for all SNRs with detections, and list these values in Table 