Kennicutt 1991). The SNR had been observed previously in FUV absorption with $\fuse$, using the Luminous Blue Variable HD 5980 as a background source (Koenigsberger et al. 2001; Hoopes et al. 2001), but no FUV emission had been detected. Indeed, [*no optical shell or emission from the SNR is evident in images of the region*]{}, and only extremely faint optical emission from the SNR can be detected in H$\alpha$ echelle data (Chu & Kennicutt 1988; Danforth et al. 2003). The SNR is an X-ray source (Wang & Wu 1992; Yokogawa et al. 2000; Nazé et al. 2002), but with a luminosity of only $\rm L_{x}(0.3 - 10 ~ keV) \simeq 1.4 \times 10^{35} ~ \LUM$ (Nazé et al. 2002) is certainly not in the class that would make it a priority FUV target. It is unlikely that an FUV observation of this SNR would have ever been attempted had the serendipitous spectrum not been obtained, and yet this is a bright FUV emission source.

To understand the systematics of ultraviolet emission from a wider sample of SNRs, and in particular to investigate the properties of more typical SNRs, we are conducting an FUV survey of Magellanic Cloud SNRs that is 