deletions | additions       diff --git a/subsection_A_hint_of_a__.tex b/subsection_A_hint_of_a__.tex  index 6f1f394..88dfe80 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{As mentioned described  in Section \ref{subsubsec_main_osc}, the intrinsic observed mode linewidths is $0.3-0.4 $0.4  \ \mu \rm{Hz}$, which is about three four  times wider than expected. To quantify how likely it is for oscillation modes like this to overlap one another, we use the ELC model results from Section \ref{all-eclipse} to calculate distributions of expected $\Delta \nu$ for each star. We find that 89\% of the time, $|\Delta \nu_1 - \Delta \nu_2| < 0.4 \ \mu \rm{Hz}$. 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.