deletions | additions       diff --git a/Mode Visibility.tex b/Mode Visibility.tex  index 7c14e28..616ac20 100644  --- a/Mode Visibility.tex  +++ b/Mode Visibility.tex 
...
To estimate the reduced mode visibility due to energy loss in the core, we assume any mode energy which leaks into the g mode cavity is completely lost. The mode then loses a fraction $T^2$ of its energy in a time $2 t_{\rm cross}$, where $t_{\rm cross}$ is the wave crossing time of the acoustic cavity. We show (see Supplementary Material) that the ratio of visibility between a suppressed mode and its non-suppressed counterpart is   \begin{equation}  \label{eqn:vis}  \frac{V_{\rm sup}^2}{V_{\rm norm}^2} = \bigg[1 + \Delta \nu \, \tau_{0}\, \tau \,  T^2 \bigg]^{-1} \, , \end{equation}  where $\Delta \nu \simeq (2 t_{\rm cross})^{-1}$ (e.g., \citealt{Chaplin_2013}) is the large frequency separation, and $\tau_{0}$ $\tau$  is the damping time of a radial mode with similar frequency. The value of $T^2$ can be easily calculated from a stellar model, whereas the envelope life-time $\tau_{0} $\tau  \sim 10 \, {\rm days}$ \citep{Dupret_2009,Corsaro_2012,Corsaro_2015} for stars ascending the RGB. Figure 1 compares our estimate for suppressed dipole mode visibility (equation \ref{eqn:vis}) with {\it Kepler} observations \citep{Mosser_2011,Garcia_2014}. Our estimate closely aligns with the branch of stars classified by \cite{Mosser_2011} as suppressed pulsators. The striking agreement holds over a large baseline in $\nu_{\rm max}$ extending from near the luminosity bump at low $\nu_{\rm max}$ to the very early red giants KIC 8561221 and KIC 9073950 at high $\nu_{\rm max}$.  %The predicted visibility of equation \ref{eqn:vis} has no free parameters, although there is some uncertainty in the value of $\tau_0$. Additional scatter can be accounted for by a range of stellar masses, metallicities, and inclinations in the the observed sample.