Figure 1: Surface mass density (a) and velocity (b) profiles for the simulated satellite as a function of the (projected) distance from the centre, . (a), (b), red dot-dashed and blue-dashed curves distinguish the contributions from the more concentrated ( ) and more extended ( ) components, respectively, while the thick solid black shows the total values obtained for all the stars (i.e., no distinction between populations). In the left panel, the magenta dotted line shows the best-fit King profile obtained for the total distribution of stellar mass, and the numbers quoted correspond to the derived core and tidal radii, respectively. The right panel shows the circular velocity (black dashed) plus the line-of-sight velocity dispersion profiles associated to each luminous component. Poisson uncertainties are shown for the total density and velocity dispersion profiles in our model, although they are generally smaller than the thickness of the curves. Thin lines in (a), (b) correspond to a control model, which is evolved from this initial configuration in isolation during  Gyr.