with 53 of the bins filled. Grid coverage was finer among the later spectral types, where for stars GO and later, we filled 26 of the 27 bins (9 spectral types $\times$ 3 luminosity classes). In contrast, for stars earlier than GO, only 27 of the 51 bins were covered (17 spectral types $\times$ 3 luminosity classes).

The 85 individual stars in our H–band survey are listed in Table \[sample\] along with relevent stellar properties taken from the Bright Star Catalogue (Hoffleit & Jaschek 1982). Additional restrictions on the sample selection included: i) v$sini$ $<$ 250 km s$^{-1}$ with exception of HR3982 (B7 V); ii) near-solar metallicity (avoiding those MK standards which exhibit spectral peculiarities due to enhanced or deficient metal abundance); and iii) no visual companions within the beam (separations $1-5$”). Our program was begun in advance of the K–band FTS atlas of WH97, and their sources are drawn in large measure from our sample. We note in Table \[sample\] the stars for which K–band spectra can be found in the WH97 digital atlas.

Table \[temp\] and Figure \[fig1\] provide additional insight into the temperature and luminosity coverage of our sample. In Table \[temp\], we list each of the 