Abstract
Using N-body simulations we study the morphological and kinematical properties of triaxial systems formed through cold gravitational collapses. Two models are considered; in one case, the supermassive black hole SBH already exists before the gravitational collapse, and in the other the SBH grows adiabatically after the collapsed system has reached virial equilibrium. Isophotal analysis along the principal projected axes shows that the SBH tends to make the isophotes more boxy than in the case without a central SBH. Also, the kinematics obtained from a Gauss-Hermite expansion shows that the central velocity dispersion increases in presence of the SBH while it remains almost constant for models without a SBH. Furthermore, the h_4 parameter is positive inside the radius of influence of the central black hole while it is negative beyond of this region. For models without a SBH h_4 > 0 at all radii. Finally, from these results we conclude that is not possible to distinguish between both models.
