In order to properly separate these important features from each other, a resolving power of $R \sim 1000$ is required. At this resolution, one can also obtain measurements of the HeI line at 5882 cm$^{-1}$ (1.700 $\mu$m). At $R = 3000$ one can resolve individual components of the AlI triplet, the Mg I doublet, and the CO bandheads, as well as the stark–broadened Brackett lines in the early–type dwarf stars (Table \[ftshband\]). An additional issue in the near–infrared is the significant contribution to shot-noise from air-glow lines. In the H–band air–glow from OH is sufficently bright and variable that they compromise $R=1000$ H–band spectral classification for very faint sources. Spectral resolution as high as $R \sim 5000$ will be required to resolve the bulk of these air–glow features and to obtain adequate SNR spectra of faint objects [^6].

In summary, we present an H–band spectral atlas at a resolving power of $R = 3000$ that spans a wide range in stellar temperature (O7-M5) and luminosity class (I-V). This spectral region contains a number of temperature and/or luminosity sensitive atomic and molecular features which will allow spectral classification to be carried out in the H-band. As an example of the efficacy 