deletions | additions       diff --git a/subsubsection_Mixed_oscillation_modes_label__.tex b/subsubsection_Mixed_oscillation_modes_label__.tex  index 054b180..93768ae 100644  --- a/subsubsection_Mixed_oscillation_modes_label__.tex  +++ b/subsubsection_Mixed_oscillation_modes_label__.tex 
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% Benoit  \revise{Finally, we 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 presence of a second oscillation spectrum cannot mimic a mixed-mode pattern because its global amplitude is too small for us to observe a mode disturbance. Only one signature of an oscillating star is visible in a period spacing diagram.}  \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. \newrevise{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}. However, the mixed modes appear to be duplets rather than higher-order splittings, doublets  which supports support  an inclination near 90 degrees.}