observations obtained in June 2005 for a zenith angle of $49\mbox{$^{\circ}$}$, regardless of the actual zenith angle of the observations. All of these observations were obtained with actual zenith angles in the approximate range of $30-50\mbox{$^{\circ}$}$. According to information presented on the DSOS website (see footnote to §\[subobs\] for web address), the corrections to the telescope efficiency introduced by the DSOS vary by up to approximately 10% across this range of zenith angles. Thus, 10% is a conservative estimate of the additional uncertainty introduced by this equipment malfunction. The flux density uncertainties for the June 2005 observations listed in Table \[properties1\] include this additional 10% uncertainty, added in quadrature to both the measurement uncertainty and 15% calibration uncertainty. The uncertainty in the peak flux for the sources observed in June 2005 also includes this additional 10%.

For properties relating to the sizes and shapes of the cores, the oversampled maps may not always give reliable results. Thus, we used the IDL procedure “hrebin,” available as part of the online IDL Astronomy User’s Library[^8], to rebin the data into Nyquist sampled maps. Sources were then extracted with Extractor, as described above, at both the half-maximum and 2$\sigma$ contours. Table \[properties2\] lists 