deletions | additions       diff --git a/subsection_A_hint_of_a__.tex b/subsection_A_hint_of_a__.tex  index 2280aee..df39161 100644  --- a/subsection_A_hint_of_a__.tex  +++ b/subsection_A_hint_of_a__.tex 
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$8.14\substack{+0.06 \\ -0.03}$ and $8.20\substack{+0.03 \\ -0.04} \ \mu\rm{Hz}$   for Star 1 and Star 2, respectively.  %The effective frequency resolution of the power spectrum for four years of \emph{Kepler} data is about $0.008 \ \mu \rm{Hz}$, and, more importantly,  \newrevise{The intrinsic observed mode line widths is about $0.5 \ \mu \rm{Hz}$, which is three times wider than typically seen in red giants. To quantify how likely it is for oscillation modes like this to overlap one another, we use the ELC model results from Section \ref{model} \ref{all-eclipse}  to calculate distributions of expected $\Delta \nu$ for each star. We find that 90\% of the time, $|\Delta \nu_1 - \Delta \nu_2| < 0.5 \ \mu \rm{Hz}$. This suggests that, if both stars do indeed exhibit solar-like oscillations, some degree of mode overlap is likely.} %Given this, the oscillation pattern from a second star (if present) should \emph{not} appear to lie exactly on top of the oscillation pattern we do see.  Searching for a second set of oscillations is motivated by the broad, mixed-mode-like appearance of the $\ell=0$ modes in Figure \ref{fig:echelle}, where mixed modes are not physically possible, and by the faint diagonal structure mostly present on the upper left side of the $\ell=1$ mode ridge. Even though oscillation modes from the two stars should not perfectly overlap, modes of degree $\ell=0,1$ of one star can almost overlap modes of degree $\ell=1,0$ of the other star.