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For applications in population synthesis, libraries of theoretical stellarspectra are often considered an alternative to template libraries of observedspectra, because they allow a complete sampling of stellar parameters. Mostattention in published theoretical spectral libraries has been devoted to thevisual wavelength range. We present a detailed comparison of theoreticalspectra in the range 1.57-1.67$\mu$m, for spectral types from A to early M andfor giants and dwarf stars, with observed stellar spectra at resolutions around3000, which would be sufficient to disentangle the different groups of latetype stars. We have selected the NeMo grids of stellar atmospheres to performsuch a comparison. We first demonstrate that after combining atomic andmolecular line lists, it is possible to match observed spectral fluxdistributions with theoretical ones very well for almost the entire parameterrange covered by the NeMo grids at moderate resolution in the visual range. Inthe infrared range, although the overall shape of the observed fluxdistributions is still matched reasonably well, the individual spectralfeatures are reproduced by the theoretical spectra only for stars earlier thanmid F type. For later spectral types the differences increase and theoreticalspectra of K type stars have systematically weaker line features than thosefound in observations. These discrepancies are traced back to stem primarilyfrom incomplete data on neutral atomic lines, although some of them are alsorelated to molecules. Improving atomic data in the near infrared is a keyelement in making the construction of reliable libraries of stellar spectra inthe infrared feasible.Comment: 17 pages, 19 figures, accepted for publication in A&

Prospects for population synthesis in theHband: NeMo grids of stellar atmospheres compared to observations