deletions | additions       diff --git a/section_Methods_subsection_Dipole_mode__.tex b/section_Methods_subsection_Dipole_mode__.tex  index a9336be..9308bfa 100644  --- a/section_Methods_subsection_Dipole_mode__.tex  +++ b/section_Methods_subsection_Dipole_mode__.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 of \dnu, \numax, and mass from \citep{Stello_2013}. \cite{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(\numax\ $-$ 2\dnu) to 
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