X-ray images of the objects. Secondly, it may be advantageous to point through the centers, where typical Doppler shifting of $\pm$30 – 150 $\VEL$ would move any SNR emissions out from under potential overlying absorptions by the host galaxy. This is an important factor for strong resonance lines such as C III $\lambda$977 and O VI, the strongest lines seen in most SNR spectra.

In practice, since published catalog coordinates were used for many of the objects, the $\fuse$ apertures did not always lie on the exact central positions. In objects with spotty optical emission, for instance, some of the Mathewson et al. (1983, 1984, 1985) coordinates are off center with respect to newer X-ray data, which tends to show the full extent of more objects. Also, in retrospect, some of the MCELS-supplied coordinates did not correspond to the object centers. In all of the SNR figures that follow, we show the actual LiF1A LWRS aperture location observed (i.e., coordinates shown in Table 2), so any miscenterings will be obvious. Since most of the objects in our survey were from 1  to 5 in extent, the LWRS apertures were usually filled with potential emission, even if modest channel misalignments or 