and have low foreground extinction. Notable but difficult observations of the Crab Nebula (Blair et al. 1992), SN 1006 (Raymond, Blair, & Long 1995; Korreck et al. 2004) and Puppis A (Blair et al. 1995) have also been performed.

The foreground galactic extinction toward the Magellanic Clouds is relatively low, but the number of SNRs observed in the FUV is still very modest (see Table 1). The young ‘core collapse’ SNRs N132D (LMC) and 1E 0102-7219 (SMC) are very bright in soft X-rays and have been studied in the UV as well (Morse et al. 1996; Blair et al. 2000a). The X-ray and optically-bright SNR N49 has received considerable attention (Vancura et al. 1992; Blair et al. 2000b; Sankrit, Blair, & Raymond 2004). However, the next brightest optical SNR in the LMC, N63A, has not been observed in the ultraviolet since the early days of the International Ultraviolet Explorer (IUE) satellite (Benvenuti, Dopita, & D’Odorico 1980) even though it should be readily detectable by modern instrumentation. Three out of four of the Balmer-dominated SNRs identified by Tuohy et al. (1982) have only recently been detected with $\fuse$ (Ghavamian et al. 2006). Not only is this a small sample, but the 