deletions | additions       diff --git a/section_Conclusions_We_have_surveyed__.tex b/section_Conclusions_We_have_surveyed__.tex  index 8ec0001..cd66acc 100644  --- a/section_Conclusions_We_have_surveyed__.tex  +++ b/section_Conclusions_We_have_surveyed__.tex 
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\section{Conclusions}  We have surveyed 44 YSOs located near the edges of MIR-identified bubbles in CS(1-0) using the GBT. Our conclusions are:  \begin{itemize}  \item We have detected CS toward 18 sources sources.  \item Using Herschel/HiGal survey data, we calculated CS abundances for these sources to be $\sim$10$^{-7}$ and range between 0.16-9.36 $\times$10$^{-7}$ $\times$10$^{-7}$.  \item Three sources show non-gaussian non-Gaussian  line-profiles with strong emission on the blue-shifted side. We interpret this profile as caused by gas infall onto a protostar. \item Two of the infall candidates (N62-1 and N90-2) are embedded in infrared dark clouds along the edge of their expanding bubbles. The combination of photometry-based YSO identification, CS-based infall, location inside an IRDC and on the edge of an expanding bubble is strongly suggestive of triggered star-formation. star formation.  \item Using a two-component model, we estimate that one infall candidate, N117-3, has an average infall speed of 0.31 km/s and a mass infall rate of 2.9 $\times$ 10$^{-5}$ M$_\odot$/yr. These numerical results are consistent with intermediate to massive star-formation.  \item Our interpretation of infall in N62-1, N90-2, and N117-3 assumes that the observed CS emission is optically thick. However, our interpretation of the asymmetric, non-Gaussian line profile in N65-2 is that there are two line-of-sight clouds contributing to the emission. It is possible that a similar mechanism could produce the profiles seen in N62-1, N90-2, and N117-3. Further observations of an optically thin line, for example $^{34}$CS, are needed to distinguish between the two possible interpretations. 
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