described our procedures for using TODCOR techniques to measure the RVs of an SB2 [e.g. @2014arXiv1402.0846L; @2012ApJ...751L..31B; @2008ApJ...689..416B], and we refer the interested reader to the discriptions therein. Our one-dimensional correlation analysis is the trivial simplification of the two-dimensional case.

Concurrently with our HRS EB observations, we observed an extensive spectral template library of known single dwarf stars using an identical HRS configuration. This library ranges in spectral type from early F through mid M. Additionally, we have supplemented this library with synthetic templates generated from the `PHOENIX`-based BT-Settl model grid [@2011ASPC..448...91A]. These synthetic models cover a much wider range of $T_{eff}$, $\mathrm{[M/H]}$, and $\log{g}$ than our observed library, although some demonstrate substantial discrepancies with observed spectra at high-resolution [@2014ApJ...782...61T] that manifest in our RV analysis as reduced correlation power. To generate a template from the BT-Settl library, we convolve the raw synthetic spectrum to the proper resolution (22,500 for APOGEE; 30,000 for HRS), and resample to 3-pixels per resolution element. We additionally apply a suite of rotational broadening kernels generated from a four parameter non-linear limb-darkening model and the appropriate stellar parameters. We do not have an observed template library for the H-band APOGEE spectra, so all APOGEE RVs 