the ratio $\rc/\rhalf$ (indicating the position of the knee in the density profile) increases systematically from dMOND to Newtonian simulations.

The circularized projected density profiles of the end-products are analyzed as described in Section \[secic\]. The best-fit Sersic indices $m_a$, $m_b$ and $m_c$ (for projections along the axes $a$, $b$, and $c$, respectively) are reported in Table 2, together with the $1\sigma$ uncertainties corresponding to $\Delta \chi^2=1$; the relative uncertainties on the best-fit Sersic indices are in all cases smaller than 5 per cent and the average residuals between the data and the fits are typically $0.05 \lsim\langle\Delta{SB}\rangle \lsim 0.2$, where $SB\equiv-2.5 \log [I(R)/\Ie]$. The fitting radial range $0.1\,\lsim\, R/\Re\,\lsim\, 10$ is comparable with or larger than the typical ranges spanned by observations (e.g., see Bertin, Ciotti & Del Principe 2002). In agreement with previous investigations, we found that the Newtonian collapse produced a system well fitted by the de Vaucouleurs (1948) law. MOND collapses led to systems with Sersic index $m<4$, down to $m\sim2$ in the case of the dMOND collapse. Figure \[fig2d\] (bottom) shows the circularized (major-axis) projected density profiles for the end-products of simulations D, M1 and N together with their best-fit Sersic laws ($m=2.87$, $m=3.20$, and 