deletions | additions       diff --git a/subsection_Mass_distributions_label_sec__.tex b/subsection_Mass_distributions_label_sec__.tex  index fd669b5..e70165c 100644  --- a/subsection_Mass_distributions_label_sec__.tex  +++ b/subsection_Mass_distributions_label_sec__.tex 
...
\subsection{Mass distributions}  \label{sec:mspec}  Figure \ref{fig:massdist} plots the cumulative mass distribution functions, normalized by the survey area for five different radial bins through the galaxy. We present two representations of these data. The normalization to equal area bins mimics the binning used in \citet{Adamo_2015} to facilitate comparison with that work. That binning divides the galaxy into regions with equal area in the original optical data. The data set we analyze here does not span the full range of angles around the galaxy, though the areas are still significant fractions of the galaxy (see Figure \ref{fig:tmaxmap}). The mass distributions clearly evolve over the face of the galaxy and several of the bins show some evidence for truncation at high masses. To emphasize the changing nature of mass distributions, we also plot the distributions binned radially into groups with equal total mass ($M_{\mathrm{tot}}=1.4\times 10^{8}$). This binning showsthat  the evolution of how the same amount of molecular gas  mass distributions change significantly is distributed in each region,  with the distribution in the center of the M83 having significantly higher mass clouds than the outer disk. Of note, the mass distribution of clouds between $1.0\mathrm{~kpc}