The proper motion dispersion profile for our best-fit IMBH model is shown in black. Shaded magenta and green are the observed proper motions for major and minor axes taken from vdMA10 but with respect to the kinematic center. The model proper motion dispersions for a cluster containing an IMBH mass of 2% of the stellar mass has a higher velocity dispersions than the observed one in the central 10′′. The residual is illustrated only for major axis data for clarity.