deletions | additions       diff --git a/Table_ref_tab_masses_shows__.tex b/Table_ref_tab_masses_shows__.tex  index 68f8db7..399ccce 100644  --- a/Table_ref_tab_masses_shows__.tex  +++ b/Table_ref_tab_masses_shows__.tex 
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Table \ref{tab:masses} shows the variation in the characteristic masses for the ISM in the system using the radial profiles described above. While the Jeans mass remains high across the galaxy, the Toomre mass using the full epicyclic frequency calculation shows reasonably  good agreement with the upper mass limits for the GMCs as well as a significant radial decrease. This points to shear regulation being important at setting the upper mass scale for molecular clouds as well as their lifetime \citep[e.g.,][]{Meidt_2015}. The Toomre masses in the inner regions of the galaxy are likely overestimates since the L04b rotation curve and low-resolution THINGS data we use here neglect the complex dynamical environment in the inner 500 pc of M83 associated with its double nucleus \citep{Sakamoto_2004,Rodrigues_2009}. Furthermore the shear rate in the bar will be larger than predicted from the circular velocity curve alone owing to the substantial non-circular motions. In these two regions, the Toomre mass limits will be overestimates of the fragmentation scale in the region.  The  characteristic masses of the clusters should be linked to the characteristic masses in the ISM \citep{Diederik_Kruijssen_2014} with the cluster mass given as: \begin{equation}  M_{c,\mathrm{cluster}} = \epsilon \Gamma M_{c,\mathrm{GMC}},  \end{equation}  where $\epsilon$ is the star formation efficiency (dimensionless) and $\Gamma$ is the bound cluster formation efficiency. The cluster formation efficiency has been observed in M83 to decrease with radius \citep{Silva_Villa_2013} with typical scales of $\sim$10\%. Star formation efficiencies of molecular clouds are $\sim 10\%$, consistent with cloud lifetimes of $\sim 30$ Myr \citep{Fukui_2010, Meidt_2015}, star formation per free fall time of $\epsilon_{\mathrm{ff}} = 10^{-2}$ \citep{Krumholz_2011}, and free fall times of 3 Myr (Table \ref{tab:masses}). Combining these two efficiencies suggests the observed values of $M_{c,\mathrm{cluster}}/ M_{c,\mathrm{GMC}} = 10^{-2}$ is largely consistent with expectations. For $R_g>0.5$~kpc, the observed cluster formation efficiency $\Gamma$ drops by a factor 3 over the region studied \citep{Silva_Villa_2013}, but the internal conditions of the molecular clouds do not change significantly in the disk of the galaxy. The clouds all show roughly constant properties including turbulence, surface density, internal pressure and free-fall time (Figure \ref{fig:radial}, Table \ref{tab:masses}) \ref{tab:masses}).