deletions | additions       diff --git a/Mode Visibility.tex b/Mode Visibility.tex  index bdfec35..3a193c3 100644  --- a/Mode Visibility.tex  +++ b/Mode Visibility.tex 
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where $\Delta \nu \simeq (2 t_{\rm cross})^{-1}$ \cite{Chaplin_2013} is the large frequency separation between overtone modes, and $\tau$ is the damping time of a radial mode with similar frequency. The value of $T^2$ can be calculated from a stellar model, whereas {\bf $\tau \approx 5 \! - \! 10 \, {\rm days}$} {\bf \cite{Dupret_2009,Corsaro_2012,Grosjean_2014,Corsaro_2015} } for stars ascending the RGB.  Most observed modes are near the frequency $\nu_{\rm max}$, which is determined by the evolutionary state of the star. On the RGB, more evolved stars generally have smaller $\nu_{\rm max}$.   Figure \ref{fig:moneyplot} compares our estimate for suppressed dipole mode visibility (equation \ref{eqn:vis}) with {\it Kepler} observations \cite{Mosser_2011,Garcia_2014}. The {\bf objects classified identified  by \cite{Mosser_2011} assuppressed  depressed dipole modes (DDM)} modes}  stars lie very close to our estimate. The striking agreement holds over a large baseline in $\nu_{\rm max}$ extending from the very early red giants KIC 8561221 \cite{Garcia_2014} and KIC 9073950 at high $\nu_{\rm max}$ to near the luminosity bump at low $\nu_{\rm max}$. We conclude that the cores of stars with suppressed {\bf depressed}  dipole modes efficiently trap waves tunneling through the evanescent region. This is further supported by the their  normal $\ell=0$ mode visibilityin suppressed pulsators  (because radial modes do not propagate within the inner core) and the lack (or perhaps smaller degree) of suppression {\bfdepression}  observed in $\ell=2$ modes by \cite{Mosser_2011}, because quadrupole modes have a smaller transmission coefficient $T$. An additional consequence is that the larger effective damping rate for suppressed modes will lead to larger line widths in the oscillation power spectrum. The linewidth of a suppressed mode is $\tau^{-1} + \Delta \nu T^2_{\ell}$ and is generally much larger than that of a non--suppressed mode. The suppressed dipole modes in KIC 8561221 \cite{Garcia_2014} indeed have much larger linewidths than non-suppressed dipole modes in similar stars. 
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