deletions | additions       diff --git a/The_nuclear_clouds_0_0__.tex b/The_nuclear_clouds_0_0__.tex  index fa49f66..8a07952 100644  --- a/The_nuclear_clouds_0_0__.tex  +++ b/The_nuclear_clouds_0_0__.tex 
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The nuclear clouds (0-0.45 kpc) are the only bin well represented by a truncated power law. Adamo et al. (2015) excluded this inner bin due to the high luminosity gradient and the more active star formation. The stellar clusters, in contrast, 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, but in relation to the stellar clusters in M83 the indices are larger and do not consistently increase outwards (Table 1) \cite{Fukui_2010}.  \begin{table}   \begin{tabular}{ c c c } c c}  Bin (kpc) & GMC $\alpha$ & GMC M$_c$ $M_c$  ($10^6$ M$_\odot$) & Stellar cluster $\alpha$ & Stellar cluster M$_c$ $M_c$  ($10^5$ M$_\odot$) \\ 0-0.45 & -1.37 & 33.35 & N/A & N/A \\   0.45-2.3 & -1.65 & 4.95 & -1.90 & 4.00\\   2.3-3.2 & -1.72 & 3.92 & -2.20 & 1.00\\   3.2-3.9 & -1.75 & 3.34 & -2.20 & 0.55\\   3.9-4.5 & -1.84 & 2.24 & -2.70 & 0.25\\   \end{tabular}   \caption{The power law indices $\alpha$ and truncation masses M$_c$ $M_c$  for giant molecular clouds and stellar clusters (from Adamo et al. 2015) in bins of equal area. The properties were derived for clouds more massive than 3e5 M$_\odot$, and clusters more massive than 5000 M$_\odot$.} \end{table}