deletions | additions       diff --git a/section_Methods_subsection_HOW_WE__.tex b/section_Methods_subsection_HOW_WE__.tex  index 9d143e6..d9a9ca6 100644  --- a/section_Methods_subsection_HOW_WE__.tex  +++ b/section_Methods_subsection_HOW_WE__.tex 
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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)  and adopted the values ofthe large frequency separation,  \dnu,the  frequency of maximum power,  \numax, and mass from \citep{Stello_2013}. To correct the spectrum for the background noise, we measured and subtracted a linear  slope anchored on the median power on either side of the central  power excess, defined by the frequency ranges 0.75(4\dnu\ $-$ \numax) to 
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the convective core in more massive stars, which generates stronger  magnetic fields that survive after hydrogen burning ceases in the core.   [Jim/Matteo elaborate?]