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We investigate the interaction history of the M31 sub-group of galaxies bycomparing surface photometry of its two nearest satellites, M32 and NGC 205,with N-body simulations of satellite destruction. The recent discovery of agiant stream in M31's outer halo, apparently pointed towards M32 and NGC 205,makes such an investigation particularly relevant. The observational componentof this study is based on 1.7 x 5.0 degree B- and I- band CCD mosaic imagescentered on M31 and covering both satellites. The simulation component of thisproject is based on the analysis of single-component, spherical modelsatellites that are tidally disrupted through interactions with their parentgalaxy. Generic features of the simulations include an excess in the surfacebrightness profile at large radii, a depletion zone at intermediate radii, andisophotal elongation and twists that are coincident with breaks in thebrightness profile. The satellites M32 and NGC 205 display most of thesefeatures consistently across the B and I bands, strongly suggestive of tidalinteraction and probable stripping by M31. We discuss what these observedfeatures can tell us about the satellites' orbital parameters and histories.Specifically, M32 is found to be on a highly eccentric orbit and away frompericenter. Investigating M32's unusual combination of high surface brightnessand low luminosity (the hallmark of compact ellipticals), we conclude onempirical grounds that M32 is not likely to be the residual core of atidally-stripped normal elliptical galaxy as has been suggested, but ratherthat its precursor was intrinsically compact.Comment: 43 pages, including 16 figures, and 2 tables; accepted for  publication in AJ; minor changes made to the tex

Tidal Interaction of M32 and NGC 205 with M31: Surface Photometry and Numerical Simulations