deletions | additions       diff --git a/subsubsection_Mixed_oscillation_modes_label__.tex b/subsubsection_Mixed_oscillation_modes_label__.tex  index 3886620..6b2431f 100644  --- a/subsubsection_Mixed_oscillation_modes_label__.tex  +++ b/subsubsection_Mixed_oscillation_modes_label__.tex 
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\textbf{PAUL}  \revise{Due to the noise and damped oscillation, it is difficult to unambiguously derive the mixed mode pattern, described by Mosser+ (2012). Therefore we searched for a stars, which PSD resembles the oscillation spectrum of KIC 9246715. A good match was found with the star KIC 11725564 (Figure \ref{}), resembling well the radial and quadrupole modes, as well as the mixed mode pattern.  Calculating the autocorrelation of the oscillation spectrum of KIC 9246715 from which the radial and quadrupole mode have been pre-whitened and which is converted into period, we find a week, broad peak at about 80 seconds. seconds [this is observed $\Delta P_{\rm{obs}}$, not $\Delta \Pi_1$].  A similar result of 87 seconds is found for KIC 11725564, whereby the signal is naturally much cleaner due to the higher mode amplitudes. This period spacing, derived from the autocorrelation corresponds to the observed period spacing, as defined by Bedding+ (2011) and Mosser+ (2011) and indicates that the star is indeed likely to be a secondary clump star.} \textbf{BENOIT}  \revise{The use of the universal red giant oscillation pattern \citep{2011A&A...525L...9M} for analyzing the spectrum of KIC 9246715 provided the measurement of the large separation $\Dnu = 8.33 \pm 0.04\,\mu$Hz, but also exhibited many supernumerary peaks. As soon as it was clear that these peaks cannot be mixed modes, the hypothesis of a binary companion was tested. Again, the universal oscillation pattern allowed us to allocate the supernumerary peaks to a pressure-mode oscillation pattern based on $\Dnu= 8.62\pm 0.04\,\mu$Hz. The spectra are globally interlaced, with the dipole modes of one component close to the radial modes of the other component, and conversely.