LWRS aperture position and orientation for each observation. Since the LWRS aperture is 30 in size, this also provides the spatial scale for each image. $\fuse$ data segments near the O VI and C III regions are shown in separate panels of each Figure. Because we are searching for faint emission lines, we found it beneficial to bin most data sets over 8 CalFUSE 3.0.7 pixels ($\sim$30 $\VEL$) for display in the Figures. A brief discussion of each detected SNR is presented in the Appendix.

As can be seen in Figures 2 - 16, the line profiles exhibit a wide range of shapes. Some are broad (several hundred $\VEL$), some narrow (only slightly above the filled aperture resolution), and some are multi-peaked. The O VI $\lambda$1032 profile is most instructive, as it is often the strongest line seen and has relatively good signal-to-noise ratio. These figures each contain horizontal bars with tick marks that indicate the positions of [*potential*]{} ISM absorption features, primarily $\rm H_2$ and O I lines. The bar marked “MW" (for Milky Way) shows the Galactic rest frame, and the other bar is shifted to the rest frame of the appropriate Magellanic Cloud (+275 $\VEL$ for LMC; 