and on-orbit performance information are provided by Moos et al. (2000; 2002) and Sahnow et al. (2000).

The $\fuse$ survey strategy involved a standard 10 ks request on each object. These faint emission line sources could all be observed in time-tagged mode. The size of the LWRS apertures plus the sensitivity of the $\fuse$ detectors combine to provide exceptional diffuse source sensitivity compared with other FUV spectrographs that have been flown. For instance, a nominal 10 ks observation would detect emission in O VI $\lambda$1032 that is 100 times fainter than the bright LMC SNR N49 (Blair et al. 2000; Sankrit et al. 2004), with limiting flux levels near $\rm 5 ~\times ~ 10^{-15} ~ ergs~cm^{-2}~s^{-1}$. Actual observation times ranged above and below the nominal 10 ks request, at the convenience of the $\fuse$ schedulers. (See discussion below and Table 2.)

The intent of the survey was to place the LiF1A LWRS aperture at or near the projected center of each SNR. This strategy had two primary motivations. First of all, to do anything other than this would apply a bias to our survey that was not desirable. We did not want to point at features selected from optical or 