for the first time, we can compare with the scaling relations of elliptical galaxies MOND models produced by a formation mechanism, yet as simple as the dissipationless collapse.

In this Section we consider the end-products of simulations M1, M2, and M4. As already discussed in Section \[secsim\], each of the three systems corresponds to a family with constant ${{M_*}}/{r_*}^2$. This degeneracy is represented by the straight dotted lines in Fig. \[figfp\]a: all galaxies on the same dotted line have the same $\kappa$ value. This behavior is very different from the Newtonian case, in which the result of a N-body simulation can be placed anywhere in the space $\Re-{{M_*}}$, by arbitrarily choosing ${{M_*}}$ and ${r_*}$. For comparison with observations, the specific scaling laws represented in Fig. \[figfp\] (thick solid lines) are the near-infrared $z^*$-band Kormendy relation $\Re \propto
{{M_*}}^{0.63}$ and FJ relation ${{M_*}}\propto\sigma_0^{3.92}$ (Bernardi et al. 2003a), and the edge-on FP relation in the same band $\log \Re = A \log \sigma_0 + B \log ({{M_*}}/ \Re^2) +const$ (with $A=1.49$, $B=- 0.75$; Bernardi et al. 2003b), under the assumption of luminosity-independent mass-to-light ratio.

The physical properties of each model are determined as follows. First, for each model (identified by a value 