deletions | additions       diff --git a/Analysis.tex b/Analysis.tex  index cfc0a61..be9cb71 100644  --- a/Analysis.tex  +++ b/Analysis.tex 
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\kappa = \kappa_{1.3mm} \left(\frac{\lambda}{1.3mm}\right)^{-\beta}\\  \end{equation}  where 3.73 x 10$^{-16}$ converts the surface brightness from Jy/(1" 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 OH94, $\theta$=15.0", 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$_{tot}$. This results are summarized in Table X, where we report the flux density at 5 wavelength bands for each CS dedection, the best-fit temperature, the total column density and the CS abundance. 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 the Herschel band emission not fitting nicely within the GBT beam. As a result, 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.  \begin{table}[] \begin{table}  \begin{tabular}{rrrrrrrrr}  Name & Blue (Jy) & Red (Jy) & PSW (Jy) & PMW (Jy) & PLW (Jy) & Temperature (K) & Total Column Density ($\times$10$^{21}$ cm$^{-2}$) & CS Abundance ($\times$10$^{-7}$)\\  N62-1 & 31.1 & 106.4 & 157.4 & 78.0 & 30.6 & --- & --- & --- \\ 
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