Despite the usefulness of NH$_3$ as a tracer of dense gas, angular resolution of the GAS data is relatively low. At NH$_3$'s 23.7GHz emission regime, for example, the Green Bank Radio Telescope has a beam size of 32", which is larger than many of the cores in these regions (which are typically between 10" and 40"). Figure 7 shows the beam size of GAS as the vertical dashed line, in relation to the sizes of cores shown on the horizontal axis.  This disparity in size makes identifying cores and defining their radii with high precision extremely difficult. Mass determination is also challenging, since non-uniform NH$_3$ abundances can introduce a great deal of uncertainty into total mass approximations using NH$_3$ (1,1) continuum emission. Hence, GAS data must be supplemented with sub-millimeter data from the James Clerk Maxwell Telescope (JCMT) at 850 $\mu$m and 450 $\mu$m, which detects material with much finer resolution, with beam sizes of 14.1" at 850 $\mu$m and 9.6" in 450 $\mu$m \citep{Dempsey13}. Very extensive fields in Ophiuchus, Taurus, and Perseus were surveyed by JCMT as part of the Gould Belt Survey (GBS) \citep{WardThompson07}, which also covered all other notable Gould Belt clouds visible from the telescope's northern hemisphere vantage point on the summit of Mauna Kea. Source identification was therefore run on a region that is much more extensive than the GAS data, and subsequently, any sources found in JCMT data that were out of bounds in GAS data were simply omitted from our analysis. Details on the source extraction and related parameters are explained in depth below in Sections 2.3-2.5.