deletions | additions       diff --git a/sectionAnalysis__sub.tex b/sectionAnalysis__sub.tex  index a05034d..6671148 100644  --- a/sectionAnalysis__sub.tex  +++ b/sectionAnalysis__sub.tex 
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\kappa = \kappa_{1.3mm} \left(\frac{\lambda}{1.3mm}\right)^{-\beta}\nonumber\\  \end{eqnarray*}  where {\bf m$_H$ is the mass of hydrogen} and 3.73 x 10$^{-16}$ converts the surface brightness from Jy/(1\arcsec beam) to SI units. We make the following assumptions: $\kappa_{1.3mm}$ = 0.11 $\frac{m^2}{kg}$, appropriate for ice-covered dust grains from \citet{1994A&A...291..943O}, $\theta$=15.0\arcsec , the beamsize of the GBT at 49 GHz, the mean molecular weight $\mu$ = 2.3 and dust to mass ratio $R_d$ = 1/100. Note that B$_\nu$, B$_{mod}$ and $\kappa$ all require a choice of frequency or wavelength. However, these dependencies cancel in the final calculation of N$_{tot}$. These results are summarized in Table \ref{mbb}, where we report the flux density at five wavelength bands for each CS detection, the best-fit temperature, the total column density and the CS abundance. We estimate the error in determining the extended flux to be dominated by defining the edge of the object. {\bf These sources all appear extended in the Herschel bands and some lie is confused regions. Thus, the gas sampled by FIR and CS are likely different. This difference should lead to a cautious association between the dust temperatures and the CS emission. As a rough benchmark, we estimated the effect of a 20\% change up or down in FIR flux on the calculated properties. The results where were  a change of 4 K in temperature and 20\% in column density.} For those sources where the modified blackbody model was a poor fit, as judged by eye, we have excluded the temperature, column density and abundance. The cause for the poor fit in these cases appeared to be caused by emission extending well outside the the GBT beam. For these poorly-fit sources, the fluxes reported here probably do not represent the emission from the same object. For those sources with a double-Gaussian CS line profile, we add the CS column densities calculated using both Gaussians. If this shape is caused by optical depth effects, as we discuss below, than the reported column density would be a lower limit.