post-processing beyond that provided by the APOGEE pipeline. We use a low order polynomial to remove continuum and normalize each spectrum. Residuals caused by imperfect correction of telluric absorption and sky emission are present in most pipeline reduced APOGEE spectra; we manually correct these by interpolating over neighboring pixels. The pipeline version used for the DR10 release flagged wavelengths with suspected bad pixels by setting their flux to zero. This flagging complicates our RV measurements because a cross-correlation analysis interprets such pixels as having strong, discrete signal that is not present in correlation templates, which reduces the overall amplitude of a real correlation signal. We interpolate over these regions to minimize their impact.

The HET High-Resolution Spectrograph\[hrs\]
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The small number of visits obtained by APOGEE in each of our fields are, by themselves, inadequate for deriving stellar mass at the 3% level for most of our EBs, but the infrared bandwidth provides essential leverage on the low-mass companions in high-contrast systems. Consequently, for 55 of our EBs (Table \[ebsampletable\], column 7) we supplemented the APOGEE spectroscopy with optical spectroscopy from the Hobby-Eberly Telescope to achive higher precision in spectroscopic orbital determination for the primary star. The High-Resolution Spectrograph [@1998SPIE.3355..387T 