deletions | additions       diff --git a/section_Conclusions_begin_itemize_item__.tex b/section_Conclusions_begin_itemize_item__.tex  index d92a618..f362bd3 100644  --- a/section_Conclusions_begin_itemize_item__.tex  +++ b/section_Conclusions_begin_itemize_item__.tex 
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\section{Conclusions}  \begin{itemize} We present a cloud-based analysis of the molecular gas in M83 as observed by ALMA. We compare the results of the cloud decomposition to the properties of the cluster population, searching for a connection between the structural organization of the molecular gas and the changing cluster properties. Based on this analysis, we reach the following conclusions:  \begin{enumerate}  \item GMCs follow the Larson Law type scalings in the galaxy  \item Nuclear clouds have higher surface densities and line widths, but still appear to be virialized.  \item We find good evidence for a characteristic mass in the mass distributions parameterized as a exponential cutoff 
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\item There is good correspondence between the truncation mass in clouds and the truncation mass for cluster  \item There is good correspondence between the truncation mass in clouds and Toomre mass  \item There is not a good correlation with Jeans mass suggesting that shear-regulated disk instabilities set the mass truncation in clouds and then those clouds go on to form stellar clusters with a roughly constant cluster formation efficiency of $\epsilon \approx 0.01$ (XXX Calculate this for reals)  \end{itemize} \end{enumerate}