$m=4.21$, respectively), and the corresponding residuals. Curiously, NLC06 found that low-$m$ systems can be also obtained in Newtonian dissipationless collapses in the presence of a pre-existing dark-matter halo, with Sersic index value decreasing for increasing dark-to-luminous mass ratio.

### Kinematics {#seckin}

We quantify the internal kinematics of the collapse end-products by measuring the angle-averaged radial and tangential components ($\sigma_r$ and $\sigma_{\rm t}$) of their velocity-dispersion tensor, and the anisotropy parameter $\beta(r) \equiv 1 -0.5\sigma^2_{\rm
t}/\sigma^2_r$. These quantities are shown in Fig. \[fig3d\] for simulations D, M1, and N. We note that the $\sigma_r$ profile decreases more steeply in the Newtonian than in the MOND end-products, while it presents a hole in the inner regions of the dMOND system. In addition, the dMOND galaxy is radially anisotropic ($\beta\sim0.4$) even in the central regions, where models N and M1 are approximately isotropic ($\beta \sim 0.1$). All systems are strongly radially anisotropic for $r\gsim\rhalf$. For each model projection we computed the line-of-sight velocity dispersion $\sglos$, considering particles in a strip of width $\Re/4$ centered on the semi-major axis of the isophotal ellipse. The line-of-sight velocity-dispersion profiles (for the major-axis projection) are plotted in the top panels of Fig. \[fig2d\]. The Newtonian profile is 