miscenterings were present. A number of the spectra are impacted to some degree by stellar emission, which affects our ability to sense the presence of potential faint emission features. Strong emission, if present, is still visible even if modest stellar contamination is present.

To date, 39 objects out of the 50 potential targets have been observed, all but one (SNR 0104-723) in the LMC. The distribution of these objects across the face of the LMC in shown in Figure 1, where detections and non-detections are indicated with separate symbols. Table 2 summarizes the targets observed and the results in terms of detections and non-detections. The details of the spectral analysis and search for SNR emission lines are described in the next section.

Analysis and Discussion
=======================

Each $\fuse$ data set has been reprocessed with the most current version of the CalFUSE pipeline publicly available at the time of our analysis, CalFUSE 3.0.7. The output from this version of CalFUSE makes it trivial to inspect both the total data sets and the orbital-night only time periods. The total data sets were inspected first. However, scattered light and backscattered solar line emission can cause confusion in the total data sets, especially for 