deletions | additions       diff --git a/section_Conclusions_We_have_surveyed__.tex b/section_Conclusions_We_have_surveyed__.tex  index 304dc28..faedb61 100644  --- a/section_Conclusions_We_have_surveyed__.tex  +++ b/section_Conclusions_We_have_surveyed__.tex 
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\item Three sources show 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.  \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, $\^{34}$CS,  are needed to distinguish between the two possible interpretations. \end{itemize}  The three infall candidates are promising sources for further study to better determine the mechanisms involved in triggered star-formation. The two candidates embedded in IRDCs are especially promising and are being mapped in a follow-up study (Devine et al., in prep.). 
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