factor of two greater than the spectra of Dallier et al. (1996). Secondly, the spectral resolution is fixed by the path difference scanned with the interferometer so we were able to chose the highest resolution possible and achieve S/N in excess of 75 for the majority of our sources. [^3] Finally, because of the novel background subtraction algorithm of the 4m FTS described below, we were able to observe the brightest stars in our sample ($H < 3.0^m$) during good daytime conditions (typically mornings). Combining daytime observations with targeted nighttime observations of key faint sources, the FTS provided a uniform set of high quality spectra for a large sample of spectral standards.

Our observing program included simultaneous spectral coverage in both the J–band and the H–band. However, the J–band data presented difficulties which made it expeditious to focus our initial effort on the H–band. The primary problems with the J-band spectra were; i) the inherent difficulty in data reduction due to rapid temporal variations in telluric water vapor absorption; and ii) and the relative paucity of strong features which would allow spectral classification over the full range of stellar temperature and luminosity. We defer discussion of the J–band spectra to 