  We present 1.1, 1.6, and 2.2 micron images of the cores of the Local Group
galaxies M 31 and M 32 obtained with the Near Infrared Camera and Multi-Object
Spectrometer (NICMOS) instrument of the Hubble Space Telescope. These images
are also compared to optical images of the galaxies obtained with the HST Wide
Field Planetary Camera 2 (WFPC2). In M 31 the nucleus remains distinctly
asymmetric in all of the infrared bands, with no evidence of concentrated dust,
although the distinction between the two nuclei, P1 and P2, is not as strong as
in the WFPC and WFPC2 images. This result is nonetheless consistent with the
model of the nucleus as an eccentric stellar disk produced by the dynamical
influence of a central supermassive black hole. Several individual M-giant
stars are detected within ~ 3" of the nuclei, and may represent stars that have
escaped from the disk and phase-mixed around the nuclear center of mass. In M
32 we also do not find strong evidence of dust, and the brightness profiles
within the central ~ 1" of the infrared images can be fitted by a power law of
the same form as that fitted to the optical images. The infrared color profiles
of the central few arcseconds of M 32 show no strong gradients, and indicate a
population dominated by K-giant stars. This is consistent with recent
groud-based spectroscopy and photometry of the core region, which similarly
show no strong gradients in age or metallicity within its stellar population.
