  We review the field of abundance determinations of elements in cool stars,
with special interest paid to determinations based on analyses of
high-resolution, 1-5 micron spectra. We discuss the current status, problems,
and challenges of exploring high-resolution, near-infrared spectra. In
particular, advantages and drawbacks are pointed out. A few examples of
current, chemical-abundance determinations are high-lighted and, finally, we
discuss the development
