a future contribution.

Spectra were collected simultaneously in the J– and H–bands with the use of a dichroic beamsplitter to separate the wavelengths longward and shortward of 1.5 $\mu$m. Each star was centered within an input aperture of 3.8 arcsec while sky background was measured through an identical aperture 50.0 arcsec away. The interferogram was scanned at a rate of 1 kHz as the path difference was varied continuously from 0.0–0.75 cm providing an unapodized resolution of 0.8 cm$^{-1}$. Data were obtained as separate scan pairs, with the path difference varied first in one direction and then the other. A forward–backward scan pair was treated as an “observation” and observations were repeated in beam–switching mode (A–B–B–A). Because the sky background from each aperture produces an interferogram shifted in phase by 180$^{\circ}$ at each set of detectors, source spectra are background subtracted in fourier space as they are collected. This permits observations of bright stars to be obtained during good daytime conditions. These beam–switched observations were repeated and scans were averaged until adequate signal–to–noise ratio (SNR) was achieved. The interferograms were transformed at Kitt Peak National Observatory yielding spectra in units of relative flux versus wavenumber ($\sigma$ in cm$^{-1}$). The transformed 