(see also Blum et al. 1997). Hanson, Conti, and Rieke (1995) have established a classification scheme in the K–band for O–B stars relying on lines of helium as well as higher ionization species obtained at $R > 1000$. For stars A through early K, the H–band may be superior to the K band in providing a large number of intermediate ionization potential species with strong features such as MgI, SiI, and FeI in addition to the numerous Brackett series features. Stars K3–M5 are probably best classified in the K–band (KH86; Ali et al. 1995; WH97) using atomic features of MgI, CaI, and NaI as well as the first–overtone CO bandheads observed at $R \sim 1000$. However we have found that these stars also have strong temperature and luminosity sensitive features in the H–band such as MgI, AlI, OH, and the second–overtone CO bandheads. The very latest–type stars ($> M5$) have very strong, broad, molecular features which can be identified at resolutions as low as $R \sim 300$. Kirkpatrick et al. 1993 (see also Jones et al. 1996) have classified stars in the I– or the J–band employing features due to VO, TiO, and FeH. In addition, broad water vapor bands 