usually set to zero at infinity for finite-mass systems, so $E<0$ for bound particles; in MOND all particles are bound, independently of their velocity, because $\phi$ is confining, and all energies are admissible. This difference is reflected in Fig. \[fignde\], which plots the initial (top) and final (bottom) differential energy distributions for simulations D, M1, and N. Given that the particles are at rest at $t=0$, the initial $N(E)$ depends only on the structure of the gravitational potential, and is significantly different in the Newtonian and MOND cases. We also note that $N(E)$ is basically the same in models D and M1 at $t=0$, because model M1 is initially in dMOND regime. In accordance with previous studies, in the Newtonian case the final differential $N(E)$ is well represented by an exponential function over most of the populated energy range (Binney 1982; van Albada 1982; Ciotti 1991; Londrillo et al. 1991; NLC06). In contrast, in model D the final $N(E)$ decreases for increasing energy, qualitatively preserving its initial shape. In the case of simulation M1 it is apparent a dichotomy between a Newtonian part at lower energies (more bound particles), where $N(E)$ is exponential, and a dMOND part at higher energies, 