deletions | additions       diff --git a/section_Methods_subsection_HOW_WE__.tex b/section_Methods_subsection_HOW_WE__.tex  index 580a6a5..dd9ee6c 100644  --- a/section_Methods_subsection_HOW_WE__.tex  +++ b/section_Methods_subsection_HOW_WE__.tex 
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\section*{Methods}  \subsection{HOW WE MADE FIG2} \subsection{Dipole-mode visibilities}  For each star in our sample we derived the frequency power spectrum as the  Fourier transform of the \kepler\ light curve (up to observing quarter 14) 
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The centres of each Lorenzian profile was fixed relative to one  another such that the one representing the $\ell=2$ modes was 0.12\dnu to the  left (lower frequency) of the $\ell=0$ profile, and the $\ell=1$ profile was  0.52\dnu to the right (higher frequency) [Huber10_800RGs]. \cite{Huber_2010}.  The shift between the model and the observed folded spectrum that gave the  larges correlation, provided the location of each mode.   %With this method the pattern of the multiple mixed  
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by the correlation with the model spectrum. The remaining region was  associated with $\ell=3$ modes (Fig. 1).  The dipole-mode visibility was derived as the integrated power of the  dipole modes relative to that of the radial modes. modes following the approach by   previous studies \citep{Mosser_2011}.  %For normal stars the integrated power in the dipole modes is typically  %about 50\% larger than for the radial modes ($V^2\simeq 1.5$)   %[This 'frequency 
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