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\subsection{Ground-based Spectra}  We have obtained several high-resolution spectra from the Apache Point Observatory (APO) 3.5 m telescope in New Mexico using the Astrophysical Research Consortium Echelle Spectrograph (ARCES). Data was taken from 2012 June through 2013 September, and we anticipate a continuation of this effort. A long time span is critical for sufficient orbital phase coverage, particularly for long-period binaries, and to account for visibility of the \emph{Kepler} field from APO. The wavelength range for ARCES is 3200--10,000 \AA \ with no gaps, and the resolution is $R \sim 31,000$. Figure \ref{phases} shows the orbital phase coverage of ARCES observations for the RG/EBs so far.  \begin{figure}[h!]   \centering  \includegraphics[width=4.5in]{all_phases_orig.png}  \caption{A %\begin{figure}[h!]   %\centering  %\includegraphics[width=4.5in]{all_phases_orig.png}  %\caption{A  timeline of ARCES spectra for the RG/EBs in Table \ref{maintable} folded on each system's orbital period. Also shown are KIC 8095275, a heartbeat star, and KIC 7955301, a triple system. Each filled symbol indicates a single observation. The primary eclipse is centered at phase zero and shaded dark gray. The secondary eclipse is light gray. Figure courtesy of Jean McKeever.} \label{phases}  \end{figure} %\label{phases}  %\end{figure}  In addition to this, our collaborators have provided high-resolution spectra from the Fred Lawrence Whipple Observatory (FLWO) 1.5 m telescope in Arizona using the Tillinghast Reflector Echelle Spectrograph (TRES) from 2012 March through 2013 April for KIC 9246715. These spectra are being used together with those from ARCES to derive an orbital solution in \citet{raw14}. High-resolution spectra are essential to extract radial velocities for each system, and if the signals from the two stars can be disentangled they can be modeled to determine atmospheric parameters such as $T_{\rm{eff}}$, $\log g$, and metallicity. This is explored in more detail in Section \ref{specanal2}.  \subsection{Ground-based Photometry}  One challenge that arises when extracting information from spectra is disentangling one star's signal from the other. To help with this, we plan to obtain ground-based multi-band photometry during both eclipses of each RG/EB whenever possible. This lets us calculate the flux ratio as a function of wavelength, which is particularly critical for systems with two components of very different stellar type. We will submit a proposal to use the NMSU 1 m telescope at Apache Point Observatory, which is robotically operated and well-suited for multiple observations of a set of targets in several bandpasses.