range of orbital periods that are challenging to observe from the ground. The majority of [*Kepler*]{} EBs are faint [only $\sim12$% of detached systems have $K_p < 12$ in @Kirk2016], and followup spectroscopy of such systems requires a combination of large telescopes and long exposure times. The *Kepler Eclipsing Binary Catalog*[^2] [@2005ApJ...628..426P; @2011AJ....142..160S; @Matijevic2012; @Conroy2014; @Kirk2016; @Abdul2016] has used [*Kepler*]{} photometry to identify thousands of EBs, and has derived extremely precise orbital periods, which greatly simplifies the process of turning individual spectroscopic measurements into an SB2 orbit.

The SDSS-III APOGEE Spectrometer\[apogee\]
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The Apache Point Observatory Galactic Evolution Experiment (APOGEE, [@Majewski2017]) is a fiber-fed, multi-object, near-infrared spectrometer that uses a volume phase holographic grating and a linear array of three Hawaii-2RG detectors to record spectra from 1.51[$\mathrm{\,\mu{}m}$]{} to 1.68[$\mathrm{\,\mu{}m}$]{} with a spectral resolution of $\lambda/\Delta\lambda\sim22,500$ [@2010SPIE.7735E..46W]. The instrument is located at Apache Point Observatory on the 2.5m SDSS telescope [@2006AJ....131.2332G; @York2000], and was commissioned in the spring and summer of 2011 for a three year survey aimed at a galactic evolution experiment [@2008AN....329.1018A; @2011AJ....142...72E]. A small fraction of the survey time ($\sim5\%$) was devoted to ancillary science programs [@2013AJ....146...81Z], which includes the [*Kepler*]{} EB program described in this paper. The 