III emission occurs for shocks with velocities above about 100 $\VEL$ while O VI emission ‘turns on’ above $\sim$160 $\VEL$, when the shock becomes effective at ionizing $\rm O^{+4}$ to $\rm O^{+5}$. Hence, we also searched for C III, which in principle could be seen even if no O VI was detectable. The SiC channels both cover the C III line region, but the SiC2A channel has higher effective area, so this channel was searched for SNR emission. Of course, channel misalignment makes the exact location of the SiC2 LWRS aperture uncertain relative to the LiF1 LWRS aperture, as described in Section 2.

Out of the 39 objects observed to date, 15 detections have been obtained, as indicated in Table 2, a detection rate of 38.5%. Summary figures showing images of each of these objects and $\fuse$ data sections are shown in Figures 2-16. Optical H$\alpha$ and \[S II\] CCD images in these figures were provided to us by the MCELS team (Smith et al. 1999), headed by R. Chris Smith of NOAO. The X-ray images have been obtained from the public HEASARC data archive for Chandra, ROSAT, XMM-Newton, and Einstein. Squares in the image panels show the nominal LiF1A 