Interactive Data language (IDL) and carries out image processing, spectral extraction, and wavelength calibration tasks. Appendix A gives a detailed description of the pipeline.

As with the APOGEE spectra, we apply several post-processing steps to our extracted HRS spectra prior to analysis. Each spectral order is continuum normalized. Strong telluric contamination is mostly restricted to isolated wavelength regions at optical wavelengths. Rather than attempt a telluric correction across our HRS bandpass, we choose to retain only those regions of the spectrum with telluric contamination of 0.5% or smaller, modulus a continuity function that preserves large unbroken chunks of spectrum. In practice, we retain eight spectral windows: 4390–5025Å, 5100–5410Å, 5475–5680Å, 5770–5855Å, 6020–6260Å, 6365–6430Å, 6620–6850Å, and 7450–7580Å. Finally, sky emission lines are removed by interpolating over neighboring pixels.

Analysis Techniques\[analysis\]
===============================

Measurement of Radial Velocities \[rvanalysis\]
-----------------------------------------------

All spectroscopy of unresolved binary stars contain the blended light of both the primary and secondary components. The S/N and the wavelength-dependent contrast ratio of an individual spectrum dictate whether that spectrum can be solved as a double-lined spectroscopic binary (SB2) or only as a single-lined spectroscopic binary (SB1). Our APOGEE spectroscopy (§\[apogee\]) was designed to exploit the NIR contrast advantage of EBs containing a 