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Spectra from MDM Observatory are used to assess Lick/IDS feature strengthgradients inside the half-light radius of the compact Local Group ellipticalgalaxy M32. All but a few (of 24 measured) indices show a statisticallysignificant gradient. Comparing with models, the index gradients indicate amean age and abundance gradient in the sense that the nucleus is a factor of2.5 younger and a factor of 0.3 dex more metal-rich than at 1 effective radius.This conclusion is only weakly dependent on which index combinations are usedand is robust to high accuracy. Stars near the M32 nucleus have a mean age andheavy element abundance [M/H] of (4.7 Gyr, +0.02), judging from models byWorthey with variable abundance ratios. This result has very small formalrandom errors, although, of course, there is significant age-metallicitydegeneracy along an (age, abundance) line segment from (5.0 Gyr, 0.00) to (4.5Gyr, +0.05). An abundance pattern of [C/M]=+0.077, [N/M]=-0.13, [Mg/M]=-0.18,[Fe/M]~0.0, and [Na/M]=+0.12 is required to fit the feature data, with afitting precision of about 0.01 dex. Model uncertainties make the accuracies ofthese values at least twice the magnitude of the precision. Forcingscaled-solar abundances does not change the age very much, but it increases therms goodness of model-data fit by a factor of 3 and broadens the allowed rangeof age to $\pm 1$ Gyr. The overall abundance pattern contrasts with largerelliptical galaxies, in which all measurable lighter elements are enhancedrelative to iron and calcium.Comment: 23 pages, 9 figures, Astronomical Journal, in pres

Balmer and Metal Absorption Feature Gradients in M32