deletions | additions       diff --git a/Table_ref_shows_the_variation__.tex b/Table_ref_shows_the_variation__.tex  index da2d0e8..8848bf0 100644  --- a/Table_ref_shows_the_variation__.tex  +++ b/Table_ref_shows_the_variation__.tex 
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\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 \cite{Silva_Villa_2013} with typical scales of $\sim$10\%. For star formation efficiencies of molecular clouds of $\sim 10\%$, 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:theoretical})