deletions | additions       diff --git a/subsection_Measurements_Uncertainties_and_varepsilon__.tex b/subsection_Measurements_Uncertainties_and_varepsilon__.tex  index 282c108..bb0b2ae 100644  --- a/subsection_Measurements_Uncertainties_and_varepsilon__.tex  +++ b/subsection_Measurements_Uncertainties_and_varepsilon__.tex 
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Most of the observational data shown in Figure \ref{fig:moneyplot} were obtained from \cite{Mosser_2012}. The additional stars KIC 8561221 and KIC 9073950 were analyzed using the same methods as \cite{Mosser_2012}. This analysis provided measured values of dipole mode visibility $V^2$, $\nu_{\rm max}$, $\Delta \nu$, and their associated uncertainties. For KIC 9073950, we used the updated KIC $T_{\rm eff}$ {\bf NEED REFERENCE} to calculate mass and its uncertainty from scaling relations. For KIC 8561221, mass and uncertainties were obtained from \cite{Garcia_2014}. To calculate values of $B_c$ for KIC 8561221 and KIC 9073950, we interpolated in $\log B_c$ between the tracks shown in Figure \ref{fig:Bc}, using the measured stellar masses. The uncertainty in $B_c$ was obtained by performing the same interpolation on the upper and lower bounds of the stellar mass.     {\bf We note that the red giant $\varepsilon$ Ophiuchi may also exhibit suppressed dipole modes. Its temperature of $\approx 4900 \, {\rm K}$, inferred mass of $1.85 \pm 0.05 \, M_\odot$ and interferometricly measured radius of $10.39 \pm 0.07 \, R_\odot$ \cite{Mazumdar_2009} yield $\nu_{\rm max} \approx 57 \, \mu{\rm Hz}$ and $\Delta \nu \approx 5.5 \, \mu{\rm Hz}$. This is consistent with the intepretation (\cite{De_Ridder_2006,Barban_2007,Mazumdar_2009}) of the peaks in its power spectrum belonging primarily to radial oscillation modes, and inconsistent with the interpretation (\cite{Kallinger_2008,Kallinger_2012}) that they are created by both radial and dipole modes. We speculate that $\varepsilon$ Ophiuchi is a suppressed depressed  dipole mode  star, explaining the apparent absence of dipole modes in its power spectrum. This interpretation is also consistent with a measured mode lifetime of 10-20 days (\cite{Kallinger_2008}), which is typical for radial modes in red giants. Non-suppressed quadrupole modes likely also contribute to the power spectrum, and may help explain the large linewidths found by \cite{Barban_2007}, who considered the peaks to be produced solely by radial modes.}