deletions | additions       diff --git a/subsection_A_hint_of_a__.tex b/subsection_A_hint_of_a__.tex  index 43921dd..ac981fa 100644  --- a/subsection_A_hint_of_a__.tex  +++ b/subsection_A_hint_of_a__.tex 
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for Star 1 and Star 2, respectively (from an inversion of Equations \ref{density} and \ref{gravity}), and the predicted $\Delta\nu_{\rm{obs}}$ are   %$8.85 \pm 0.15$ and $8.14 \pm 0.12 \ \mu\rm{Hz}$   $8.14\substack{+0.06 \\ -0.03}$ and $8.20\substack{+0.03 \\ -0.04} \ \mu\rm{Hz}$   for Star 1 and Star 2, respectively. The %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, the \newrevise{The  intrinsic observed mode line widths is about $0.5 \ \mu \rm{Hz}$. \rm{Hz}$.}  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.