deletions | additions       diff --git a/subsection_Mass_distributions_We_binned__.tex b/subsection_Mass_distributions_We_binned__.tex  index a11738a..03326cf 100644  --- a/subsection_Mass_distributions_We_binned__.tex  +++ b/subsection_Mass_distributions_We_binned__.tex 
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where $N(>M)$ is the number of clouds above a certain mass $M$, and $\alpha$ is the index. The latter expression represents the truncated power law case where $M_c$ is the maximum mass we are looking for. Using the ‘powerlaw’ package in Python, each Each  bin was fitted fit  by two distributions: an ordinary power law and a truncated power law (\ref{fig:massdist}). The distributions were constrained by a minimum mass of $3\times 10^5$ M$_\odot$ above which there is a stable fit for the whole galaxy. ‘Powerlaw’ also returned the index α The loglikelihood ratio R,  for the power law over the truncated version, and it's significance p indicate  that best there is an upper truncation mass for all bins (\ref{table:properties}).  The stellar clusters are well  described by a truncation for the three outer bins \cite{Adamo_2015}. The indices found for the GMCs are along  the data. same magnitude as those found for GMCs in other nearby galaxies \cite{Fukui_2010}.