deletions | additions       diff --git a/subsection_Searching_for_a_second__.tex b/subsection_Searching_for_a_second__.tex  index 79c9a95..37c2934 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). (I NEED TO PUT ERROR BARS ON THAT. WITH THE ERROR BARS, SPECTRA MIGHT OVERLAP PERFECTLY. I'LL DO THAT TOMORROW. P.G. 29.6.15)  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 modes are short-lived (ABOUT 23 DAYS FROM AN AVERAGE 0.5 $\mu$Hz linewidth of  $l=0$ modes linewidth), modes),  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? 
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