deletions | additions       diff --git a/subsubsection_Mixed_oscillation_modes_label__.tex b/subsubsection_Mixed_oscillation_modes_label__.tex  index 63a4967..3e8b304 100644  --- a/subsubsection_Mixed_oscillation_modes_label__.tex  +++ b/subsubsection_Mixed_oscillation_modes_label__.tex 
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%\revise{The use of the universal red giant oscillation pattern \citep{mos11} yields $\Delta \nu = 8.33 \pm 0.04 \ \mu\rm{Hz}$ for this system (Section \ref{subsubsec_main_osc}), but also shows many extra peaks which cannot be mixed modes. We therefore test the hypothesis of a binary companion. The universal oscillation pattern allows us to allocate the extra peaks to a pressure-mode oscillation pattern based on $\Delta \nu = 8.62 \pm 0.04 \ \mu\rm{Hz}$. The spectra are globally interlaced, with the dipole modes of one component close to the radial modes of the other component, and vice versa.}  \revise{Finally, we measured measure  the asymptotic period spacing with the new method developed by \citet{mos15}. The signature $\Delta \Pi_1 = 150.4 \pm 1.4 \ \rm{s}$ is very clear, despite binarity. In fact, the secondary spectrum cannot mimic a mixed-mode pattern and its global amplitude is small, so that the disturbance is limited. Only one signature is visible, which corresponds to the main component.} \revise{We conclude that the mixed oscillation modes in KIC 9246715 are indicative of a secondary red clump star.} This result is supported statistically by \citet{mig14}, who report it is more likely to find red clump stars than red giant branch stars in asteroseismic binaries in \emph{Kepler} data. This is largely due to the fact that evolved stars spend more time on the horizontal branch than the red giant branch. We note that due to the large noise level of the mixed modes, we are unable to measure a core rotation rate in the manner of \citet{bec12} and \citet{mos12}.