are different, they are qualitatively similar. A lack of sensitivity to extended emission is not surprising since, as stated in §\[subreduction\], sky emission is subtracted to first order by removing emission common to all bolometers. Thus, extended emission larger than the size of the array cannot be completely separated from sky emission. Finally, such a discrepancy in source sizes between observations with different instruments is not unique to this survey; low-mass cores observed at both 850 [$\mu$m]{} with SCUBA and 1.2 mm with MAMBO show significantly (between factors of $2-20$) larger 2$\sigma$ angular diameters at 1.2 mm than 850 [$\mu$m]{} (Young et al. 2006; J. Kauffmann et al. 2006, in preparation). Since both 850 [$\mu$m]{} and 1.2 mm are within the Rayleigh-Jeans limit, temperature effects cannot account for these discrepancies.

In reality, the discrepancy between source sizes is most likely a combination of the temperature and instrumental effects discussed above. Comparing the derived 2$\sigma$ angular diameters for sources observed with the same instrument at 350 and 450 [$\mu$m]{} could help distinguish between these two possibilities. However, only two cores were observed at both wavelengths, and, as Figure \[sizesfig2\] shows, only L483 has deep enough integrations at both wavelengths to be 