deletions | additions       diff --git a/begin_table_begin_tabular_c__1.tex b/begin_table_begin_tabular_c__1.tex  index 5cc6831..3e76683 100644  --- a/begin_table_begin_tabular_c__1.tex  +++ b/begin_table_begin_tabular_c__1.tex 
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3.2-3.9 & -1.75 & -4.12 & 0.0041 & 3.34 & & 7.59 & 2.38 & -2.20 & 0.55\\   3.9-4.5 & -1.84 & -2.69 & 0.020 & 2.24 & & 3.84 & 1.48 & -2.70 & 0.25\\   \end{tabular}   \caption{The properties of GMCs and stellar clusters (from \citet{Adamo_2015}) \cite{Adamo_2015})  in M83, for bins of equal area. Values were derived for clouds more massive than $3\times 10^5 M_\odot$, and clusters more massive than 5000 M$_\odot$. \label{table:properties}} \end{table}  We compare the characteristic masses and slopes derived from the empirical distributions to the characteristic masses produced by the Jeans instability and the Toomre instability. The Jeans instability is the characteristic fragmentation mass for a thin sheet of mass with support from a velocity distribution $\sigma_v$ and surface mass density $\Sigma$. Such a sheet will fragment into the characteristic (2D) Jeans mass for the system: