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\subsection{A hint of a second set of oscillations}  \label{subsec_second_osc}  Given that the giants in KIC 9246715 are nearly twins, we test whether it is possible that we see only one set of oscillation modes because both stars are oscillating with virtually identical frequencies. It is unlikely that two sets of solar-like oscillations lie on top of one another, because the predicted $\nu_{\rm{max}}$ for these not-quite-identical stars are $115.47 %$115.47  \pm 4.46$ and $102.9 \pm 3.46 \ \mu\rm{Hz}$ $103.4 \pm 2.1$ and $104.1 \pm 1.5 \ \mu\rm{Hz}$  for Star 1 and Star 2 respectively (from an inversion of Equations \ref{density} and \ref{gravity}), and the predicted $\Delta\nu_{\rm{obs}}$ are $8.85 %$8.85  \pm 0.15$ and $8.14 \pm 0.12 \ \mu\rm{Hz}$ $8.14 \pm 0.10$ and $8.20 \pm 0.06 \ \mu\rm{Hz}$  for Star 1 and Star 2 respectively. The effective frequency resolution of the power spectrum for four years of \emph{Kepler} data is about $0.008 \ \mu \rm{Hz}$, and, more importantly, the intrinsic observed mode line widths is about $0.5 \ \mu \rm{Hz}$. Given this, the oscillation pattern from a second star (if present) should \emph{not} appear to lie exactly on top of the oscillation pattern we do see. Searching for a second set of oscillations is motivated by the broad, mixed-mode-like appearance of the $\ell=0$ modes in Figure \ref{fig:echelle}, where mixed modes are not physically possible, and by the faint diagonal structure mostly present on the upper left side of the $\ell=1$ mode ridge. Even though oscillation modes from the two stars should not perfectly overlap, modes of degree $\ell=0,1$ of one star can almost overlap modes of degree $\ell=1,0$ of the other star.