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\subsection{Stellar parameters}\label{parameters}  We use the radiative transfer code MOOG \citep{sne73} to derive $T_{\rm{eff}}$, $\log g$, and metallicity [Fe/H]  for thetwo red giants.  \begin{itemize}  \item Identify metallicity-sensitive Fe lines in each  disentangled spectrum of each star in KIC 9246715. First, we use the Automatic Routine for line Equivalent widths in stellar Spectra \citep[ARES,][]{Sousa_2007}  with the Fe I and Fe II linelist from \citet{Yong_2005}.  ARES \citep{Sousa_2007}.  \item Then, run MOOG  \end{itemize} automatically measures equivalent widths for spectral lines which can then be used by MOOG. An excellent outline of the process is given by \citet{Sousa_2014}.  IN PROGRESS