deletions | additions       diff --git a/subsection_Searching_for_a_second__.tex b/subsection_Searching_for_a_second__.tex  index cd20358..a21c842 100644  --- a/subsection_Searching_for_a_second__.tex  +++ b/subsection_Searching_for_a_second__.tex 
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% This is about five times as wide as normal RGs.  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. To illustrate this, the observed oscillation pattern in Figure \ref{fig:seismo} (red) is shown with predicted oscillation modes based on the physical parameters of both stars in the binary (OTHER COLOR(s) - UPDATE FIGURE AND THEN WRITE ABOUT IT).  We also investigate whether the modes show any frequency modulation as a function of orbital phase by examining portions of the power spectrum spanning less than the orbital period. However, the solar-like oscillations are short-lived (and therefore broad), so it is difficult to clearly resolve Doppler-shifted modes in a power spectrum of a light curve segment. At $\nu_{\rm{max}} = 106 \ \mu \rm{Hz}$, the maximum frequency shift expected from a $60 \ \rm{km} \ \rm{s}^{-1}$ difference in radial velocity is $0.02 \ \mu \rm{Hz}$. This is less than the intrinsic mode line width, and therefore not easily observable. Write about how the ELC solutions give consistent nu-max with Star 2?  We conclude that one star truly lacks visible oscillations while the other has low-amplitude oscillations, and we are unable to definitively say which star is which. ???