deletions | additions       diff --git a/The_nuclear_clouds_0_0__.tex b/The_nuclear_clouds_0_0__.tex  index 93b0cb8..a8382fb 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. \citet{Adamo_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 \cite{Fukui_2010}. The indices are smalller than those for the stellar clusters in M83 but similarly increase outwards (Table 1).  \begin{table}   \begin{tabular}{ c c c c c c c c c}  Bin (kpc) & GMC $\alpha$ & R & p & GMC $M_c$ ($10^6$ M$_\odot$) & Largest GMC ($10^6$ M$_\odot$) & 5th largest GMC (M$_\odot$) ($10^6$ M$_\odot$)  & Stellar cluster $\alpha$ & Stellar cluster $M_c$ ($10^5$ M$_\odot$) \\ 0-0.45 & -1.37 & -18.5 & 1.2 & 33.4 & 47.7 & 22.0  & N/A & N/A \\ 0.45-2.3 & -1.65 & -33.9 & 2.2 & 4.95 & 19.4 & 6.82  & -1.90 & 4.00\\ 2.3-3.2 & -1.72 & -14.4 & 8.2 & 3.92 & 11.2 & 5.01  & -2.20 & 1.00\\ 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 power law indices $\alpha$ and truncation masses $M_c$ 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}