deletions | additions       diff --git a/Mode Visibility.tex b/Mode Visibility.tex  index a5c62d5..aa02022 100644  --- a/Mode Visibility.tex  +++ b/Mode Visibility.tex 
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\end{equation}  where $\Delta \nu \simeq (2 t_{\rm cross})^{-1}$ (e.g., \citealt{Chaplin_2013}) is the large frequency separation, and $\tau_{0}$ 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 $\tau_{0} \sim 10 \, {\rm days}$ \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}. \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.  We conclude that the cores of stars with suppressed dipole modes host a mechanism able to efficiently trap waves tunneling through the evanescent region. This is further supported by the normal $\ell=0$ mode visibility in suppressed pulsators (because radial modes do not propagate within the core) and the lack (or perhaps smaller degree) of suppression observed in $\ell=2$ modes by \citet{Mosser_2011}, because quadrupole modes have a smaller transmission coefficient $T$.