satellite to a dispersion supported galaxy (\[table:table6\]). In figure \[fig:figure9\] the decrease of the ratio due to the effect of the tides can be observed.

Projected mass surface densities and cylindrically averaged surface mass densities
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In addition to the quantities determined based on the bound amount of particles for the respective dwarf galaxies, the projected surface mass densities (PSMD) and cylindrically averaged surface mass densities (CASMD) have been determined. Unlike with the previous quantities where the nearby unbound particles are excluded from the calculations, in the PSMD and CASMD case they are included. The plots present in figures \[fig:figure2\], \[fig:figure3\], \[fig:figure10\], \[fig:figure11\], \[fig:figure12\] and \[fig:figure13\], are generated by projecting along the principal axes of the bound satellite all stellar particles inside a spherical volume of 10 kpc radius centered on the stellar density maximum of the galaxy. In the case of the CASMD calculations, the depth of the projection was reduced in order to include the stars with distances from the plane of projection smaller than 2.5 kpc. The resulting plots are available in figures \[fig:figure4\], \[fig:figure14\].

Evolution of satellites
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### Galaxy A

Originally the most massive of the studied objects, satellite A enters the host halo on 