as a normalization the following relation is used for the calculation of the scale length as a function of galaxy mass:

$$R_d = 0.4  \left( \frac{M_{vir}}{10^9 M_{sol}}\right)^{0.5} kpc.$$

For each pair of objects the parameters of the stellar component are listed in table \[table:table2\].

From the original cosmological simulation, quantities such as the virial mass and virial radius are measured (table \[table:table1\]). The virial quantities are used for determining all the parameters required for the generation of the pairs of high resolution galaxies that will be used as replacements. Namely the following quantities are determined: ($\sigma_s,r_s, r_c, r_w$) the dark matter halo quantities and ($M_{stars}, R_d$) the stellar disk quantities. The remaining free parameters are the number of dark matter particles and star particles. For all the models created both numbers were set to one million.

Stability of the galaxies
-------------------------

Each of the twelve high resolution generated objects evolve in isolation for 1 Gyr prior to their introduction in the cosmological environment. The state of the objects at the end of the isolation run can be seen in figure \[fig:figure2\] and \[fig:figure3\]. The purpose of these simulations is to verify the stability of the models and allow the system 