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

Abstract

We investigate the interaction history of the M31 sub-group of galaxies by comparing surface photometry of its two nearest satellites, M32 and NGC 205, with N-body simulations of satellite destruction. The recent discovery of a giant stream in M31's outer halo, apparently pointed towards M32 and NGC 205, makes such an investigation particularly relevant. The observational component of this study is based on 1.7 x 5.0 degree B- and I- band CCD mosaic images centered on M31 and covering both satellites. The simulation component of this project is based on the analysis of single-component, spherical model satellites that are tidally disrupted through interactions with their parent galaxy. Generic features of the simulations include an excess in the surface brightness profile at large radii, a depletion zone at intermediate radii, and isophotal elongation and twists that are coincident with breaks in the brightness profile. The satellites M32 and NGC 205 display most of these features consistently across the B and I bands, strongly suggestive of tidal interaction and probable stripping by M31. We discuss what these observed features can tell us about the satellites' orbital parameters and histories. Specifically, M32 is found to be on a highly eccentric orbit and away from pericenter. Investigating M32's unusual combination of high surface brightness and low luminosity (the hallmark of compact ellipticals), we conclude on empirical grounds that M32 is not likely to be the residual core of a tidally-stripped normal elliptical galaxy as has been suggested, but rather that its precursor was intrinsically compact.

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

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