deletions | additions       diff --git a/subsection_Mass_distributions_We_binned__.tex b/subsection_Mass_distributions_We_binned__.tex  index 03326cf..9737814 100644  --- a/subsection_Mass_distributions_We_binned__.tex  +++ b/subsection_Mass_distributions_We_binned__.tex 
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where $N(>M)$ is the number of clouds above a certain mass $M$, and $\alpha$ is the index. The latter expression represents the truncated power law case where $M_c$ is the maximum mass we are looking for. Each bin was fit by two distributions: an ordinary power law and a truncated power law (\ref{fig:massdist}). A Schechter function with index -2 was also examined for it's suitability to the data.  The distributions were constrained by a minimum mass of $3\times 10^5$ M$_\odot$ above which there is a stable fit for the whole galaxy. The loglikelihood ratio R, for the power law over the truncated version, and it's significance p indicate that there is an upper truncation mass for all bins (\ref{table:properties}). Table \ref{table:properties} also shows the index $\alpha_{GMC}$, the truncation mass $M_{c,GMC}$, the truncation mass of the Schechter function $M_{s,GMC}$, the mass of the largest cloud, the mass of the fifth largest cloud, the stellar cluster index $\alpha_{cluster}$ and the stellar cluster truncation mass $M_{c, cluster}$.  index $\alpha_{GMC}$ for the truncated power law changes below the cutoff mass, and it increases outward in the galaxy similar to the stellar cluster indices.  The stellar clusters are well described by a truncation for the three outer bins \cite{Adamo_2015}. The indices found for the GMCs are along the same magnitude as those found for GMCs in other nearby galaxies \cite{Fukui_2010}.