the object. This is performed by defining a set of particles that include both dark matter and stars inside a sphere centered on the stellar density peak and with a radius equal to two half light radii. All the bound particles of the object including the ones exterior to the two half light radii sphere are rotated such that the moment of inertia tensor, corresponding to the set of stellar particles interior to the previously mentioned sphere, is diagonalized. This process is repeated for each individual object at each epoch of measurement.

Once the satellite is identified and analysed there are a number of diagnostics that are routinely measured, as described in the following subsections. In addition to dynamical masses, dark matter masses and stellar masses (see tables \[table:table4\] and \[table:table5\] for the results at the starting and final time), the key diagnostics used to quantify the morphology of the model galaxies are the shape as measured by the axis ratios, the ratio between 1D velocity dispersion $\sigma_*$ and rotational velocity $v_{rot}$ of the stars (note that we refer here to the actual stellar rotational velocity rather than to the circular velocity), and the surface density profiles of the stars. 