spectral type and luminosity bins we have “filled”. For each bin in which there is at least one spectrum, we give the corresponding effective temperature. For most stars, we adopted the temperature scale of Tokunaga (1996), except for giants earlier than G0 where we adopted Schmidt–Kaler (1982) [^2]. Figure \[fig1\] provides a schematic illustrating the temperature and luminosity coverage for the 85 stars in our sample. In this illustration we have applied the same main sequence bolometric corrections to both dwarf (27) and subgiant (11) stars; as such they are indistinguishable in this diagram.

Observations and Data Calibration
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Observations of our 85 sample stars were obtained at the Mayall 4m telescope at Kitt Peak National Observatory during four separate observing runs from 1993–1994 (Table \[ftslog\]). We used the Fourier Transform Spectrometer (FTS) dual–output interferometer (Hall et al. 1979). The FTS was ideal for this program for several reasons. First, the wavelength coverage of the FTS is limited only by the bandpass of the blocking filters, independent of the spectral resolution. This gave us complete coverage in the J– and H–bands which would have been difficult to obtain with available grating spectrographs. For example, our H–band spectral range is a 