  We present a comparison between the observational data on the kinematical
structure of G1 in M31, obtained with the Hubble WFPC2 and STIS instruments,
and the results of dynamical simulations carried out using the special-purpose
computer GRAPE-6. We have obtained good fits for models starting with single
cluster King-model initial conditions and even better fits when starting our
simulations with a dynamically constructed merger remnant of two star clusters.
In the latter case, the results from our simulations are in excellent agreement
with the observed profiles of luminosity, velocity dispersion, rotation, and
ellipticity. We obtain a mass-to-light ratio of $M/L = 4.0 \pm 0.4$ and a total
cluster mass of $M=(8\pm 1)\times 10^6 M_\odot$. Given that our dynamical model
can fit all available observational data very well, there seems to be no need
to invoke the presence of an intermediate-mass black hole in the center of G1.
