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\revise{Equation} \ref{density} is valid only for oscillation modes of large radial order $n$, where pressure modes can be mathematically described in the frame of the ``asymptotic development'' \citep{tas80}. Even though red giants do not perfectly match these conditions, because the observed oscillation modes have radial orders $n < 10$, the scaling relations do appear to work. Quantifying how well they work and in what conditions is more challenging. This is why measuring oscillating stars' masses and radii independently from seismology is so important.  Surprisingly, when \citet{gau13} and \citet{gau14} analyzed the oscillation modes of KIC 9246715 to estimate global asteroseismic parameters, only one set of modes corresponding to a single oscillating star was found. Of the 18 oscillating RG/EBs in the \emph{Kepler} field, KIC 9246715 is the only one with a pair of giant stars (the rest are composed of a giant star and a main sequence star). The oscillation spectrum as well as its representation as an \'echelle diagram are shown in Figures \ref{fig:seismo} and \ref{fig:echelle} \revise{(see Section \ref{subsec_second_osc} for a discussion of the marginal detection of a second set of oscillations illustrated in Figure \ref{fig:echelle})}. Assuming a single oscillating star, the mode amplitudes are quite low ($A_{\rm{max}}(\ell=0) \simeq 14$ ppm, and not 6.6 ppm as erroneously reported by \citealt{gau14}) compared to the 20 ppm we expect based on mode amplitude scaling relations \citep{cor13}. In addition, the light curve displays photometric variability as large as 2\% peak-to-peak, \revise{as shown in Figure \ref{fig:lcfig2}}, which is typical of the signal created by spots on stellar surfaces. The pseudo-period of this variability was observed to be about half the orbital period, which suggests resonances in the system. \citet{gau14} speculated that star spots may be responsible for inhibiting oscillations on the smaller star, and a similar behavior was observed in other RG/EB systems. In this section, we reestimate the global seismic parameters of the oscillation spectrum that was previously identified (Section \ref{subsubsec_main_osc}), \revise{analyze the mixed oscillation modes to determine the oscillating star's evolutionary state (Section \ref{subsubsec_mixed}), identify which star is more likely to be the main oscillator exhibiting oscillations  (Section \ref{identifying}), and address the discrepancy between different surface gravity measurements (Section \ref{gravity_compare}).} \subsubsection{Global asteroseismic parameters of the main oscillator}  \label{subsubsec_main_osc}