spectrograph is stabilized in a vacuum-sealed cryostat cooled via liquid nitrogen, which minimizes thermal variations and yields a typical radial velocity precision of $100-200{\ensuremath{\mathrm{\,m\,s^{-1}}}}$ on our EB sample. APOGEE can simultaneously observe 300 targets over the telescope’s 3$^\circ$ diameter field-of-view, which is also fortuitously the approximate size of each [*Kepler*]{} module. This multiplexing capability allows us to efficiently observe many EBs with a single integration, also referred to as a *visit*. Each *visit* is typically comprised of eight consecutive eight-minute exposures, which are later combined by the APOGEE data reduction pipeline [@Nidever2015] to produce a single *visit* spectrum with a total integration time of slightly more than one hour. All analysis described in this paper utilizes APOGEE data at the *visit* level of processing.

Our ancillary APOGEE program included two fields overlapping [*Kepler*]{} modules centered on the open clusters NGC 6791 (3 *visits*) and NGC 6819 (6 *visits*). We observed a total of 42 and 67 detached EBs in each field, respectively. All spectra for this program were obtained in 2011, during the first year of survey operations, and have been publicly released as part of SDSS Data Release 10 [@2013arXiv1307.7735A].

Prior to analyzing the APOGEE spectra, we perform additional 