to remove instabilities prior to replacement. Initial discreteness noise is unavoidable, and it is known to seed waves in cold disk-like systems which could lead to mass redistribution (eg [@2011EAS....48..369M]). These often manifest themselves as transient spiral waves, although the method adopted by our initial condition generator combined with the low self-gravity of the light disks embedded in a massive halo should minimize amplification of the waves. Furthermore, two-body relaxation between more massive dark matter particles and lighter stellar particles may also lead to some spurious evolution (Mayer et al. 2001). All isolation runs were performed using the pkdgrav2 code ([@2001PhDT........21S]). The softening lengths of the particles were set according to the equation: $$\epsilon_{dark} = 0.06 \left( \frac{M_{vir}}{10^9 M_{sol}} \right)^{1/3} kpc,$$ $$\epsilon_{star} = 0.02 \left( \frac{M_{stars}}{4 \cdot 10^7 M_{sol}} \right)^{1/3} kpc,$$ And are listed in table \[table:table3\].

The baryonic distributions of the constructed galaxy models with a cusp coefficient equal to unity are presented in figures \[fig:figure2\] and \[fig:figure3\]. The previously mentioned images correspond to the objects at the end of the isolation run and at the moment of replacement. Figure \[fig:figure4\] shows the cylindrically averaged surface density at the beginning of the isolation run and at the end. Small 