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\section{Analysis}  \subsection{CS Abundance}  In order to To  calculate the abundance of CS, we first must estimate the total gas column density along each line of sight. We used FIR {\bf (60$\mu$m-600$\mu$m)} imaging taken as part of the HiGal survey. Within CASA, we measured the integrated emission in all five survey bands in regions exactly coincident with the GBT beamsize, centered at each source of CS emission. The emission was then modeled as a modified blackbody: \begin{equation*}  B_{mod} =B_0 \frac{2 h \nu^{3+\beta}}{c^3}\frac{1}{e^{\frac{h\nu}{kT}}-1}