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In this paper, we present physical parameters for the unique RG/EB KIC 9246715, which contains two nearly-identical red giants in a 171.3-day eccentric orbit. Only one set of solar-like oscillations is present, however, and the oscillations show a lower amplitude than similar giants. We find good agreement between photodynamic models and asteroseismology for the oscillating star's mass and radius, but are unable to definitively say which star is oscillating.  % placeholder text for reporting masses and radii (these values are wrong)  %($M_{\rm{Phot}} = 2.11 \pm 0.02 \ M_{\odot}$, $M_{\rm{seismo}} = 2.06 \pm 0.13 \ M_{\odot}$) and a notable discrepency in radius ($R_{\rm{Phot}} = 9.95 \pm 0.13 \ R_{\odot}$, $R_{\rm{seismo}} = 8.10 \pm 0.18 \ R_{\odot}$).  We explore how the likely presence of star spotsand moderate tidal effects  influence the oscillations, verify that the two stars are consistent with a co-evolutionary history,  and discuss how thisevolved  system can inform future detailed studies of RG/EBs. In \S \ref{data}, we describe how we acquire and process photometric and spectroscopic data, and \S \ref{rvs} explains our radial velocity extraction process. In \S \ref{atm}, we disentangle each star's contribution to the spectra to perform stellar atmosphere modeling. We then present our final orbital solution and physical parameters for KIC 9246715 in \S \ref{model}. Finally, \S \ref{discuss} compares our results with those from asteroseismology and discusses the connection between solar-like oscillations, effects such as star spots and tidal forces, and implications for future RG/EB studies.