that none of the four objects has a mass above $10^8 M_{sol}$ at z = 0 in the original ErisDark run. Therefore they are not part of the largest subhaloes at the final epoch, which can well exceed this mass at low z (Paper II, [@2014ApJ...784..161P]). In total we thus replace 6 subhalos (figure \[fig:figure1\]), of which 2 are merging during infall and the other four are accreted individually. The halo properties are listed in table \[table:table1\].

Model galaxy generation
-----------------------

The replacement models are generated using the GalactICS code ([@1995MNRAS.277.1341K], [@2005ApJ...631..838W], [@2008ApJ...679.1239W]), which generates multi-component equilibrium models of galaxies. Each model galaxy is comprised of two components: the dark matter halo and the stellar disk. It is assumed by construction that the initial model has a stellar disk since this stems from the assumption that disky dwarfs are the progenitors of dSphs, the core idea of tidal stirring. The code creates halos with negligible angular momentum and a spherically symmetric density profile as described by the relation:

$$\rho_{halo}(r) = \frac{2^{2-\gamma} \sigma_s^2}{4 \pi G r_s^2} \frac{1}{\left(\frac{r}{r_s}\right)^\gamma \left(1+\frac{r}{r_s}\right)^{3-\gamma}} \frac{1}{2} erfc \left(  \frac{r - r_c}{\sqrt{2} r_w}\right).$$

In the previous equation the scale radius and velocity scale are denoted with $r_s$ and $\sigma_s$, 