run. Based on the variation in FCF values from one observation to the next, we assign a 15% calibration uncertainty to all of our data. We investigated whether or not the beam sidelobe structure results in any dependence on the FCF values with the size of the calibrator, as the calibrators used here varied in size from $\sim 2.3$ (Neptune) to greater than 10 (Mars). No significant variation is seen, and if such a variation is present at all, it is dominated by the 15% calibration uncertainty.

Results
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The SHARC-II maps are oversampled, with pixel sizes three times smaller than those of a Nyquist sampled map. We have used these oversampled maps to derive the properties listed in Table \[properties1\]: the Barycenter position[^7], flux densities in 20 and 40 diameter apertures (S$_{20}$ and S$_{40}$, respectively), peak position, distance between Barycenter and peak positions ($\delta_{pk}$), and peak flux for each submillimeter source detected by SHARC-II. For cores with no sources detected, we list the 3$\sigma$ upper limit in each aperture. The Barycenter position is derived by extracting sources using Starlink’s Extractor, which is based on SExtractor (Bertin 2003). Extractor locates all sources above a specified intensity level, fits an ellipse 