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The identification of individual stars in crowded environments usingphotometric information alone is confounded by source confusion. However, withthe addition of spectroscopic information it is possible to distinguish betweenblends and areas where the light is dominated by a single star using the widthsof absorption features. We describe a procedure for identifying locations inkinematically hot environments where the light is dominated by a single star,and apply this method to spectra with 0.1 arcsec angular resolution coveringthe 2.1 - 2.3 micron interval in the central regions of M32. Targets fordetailed investigation are selected as areas of localized brightnessenhancement. Three locations where at least 60% of the K-band light comes froma single bright star, and another with light that is dominated by two starswith very different velocities, are identified. The dominant stars are evolvingnear the tip of the asymptotic giant branch (AGB), and have M5 III spectraltype. The lack of a dispersion in spectral-type suggests that the upper AGBwithin the central arcsec of M32 has a dispersion in J-K of only a fewhundreths of a magnitude, in agreement with what is seen at larger radii. Onestar has weaker atomic absorption lines than the others, such that [M/H] is 0.2dex lower. Such a difference in metallicity is consistent with the metallicitydispersion inferred from the width of the AGB in M32. The use of line width todistinguish between blends involving many relatively faint stars, none of whichdominate the light output, and areas that are dominated by a singleintrinsically bright star could be extended to crowded environments in othernearby galaxies.

Identifying Bright Stars in Crowded Environments Using Velocity Dispersion Measurements, and an Application to the Center of M32