  Several observations suggest the existence of super-massive black holes
(SMBH) at the centers of giant galaxies. However the mechanism under which
these objects form remains non completely understood. In this work we review an
alternative mechanism of formation of galactic SMBHs. This is, the collapse of
ultra-light scalar field configurations playing the role of dark matter halos.
Several works have studied this scenario and investigated its plausibility. The
theory of collapse of scalar field configurations into compact objects has been
extensively studied regarding to boson stars, in this work we extrapolate such
results for models of galactic halos hosting central SMBHs. We construct the
simplest setup of an ultra-light scalar field configuration laying in a
Schwarzschild space-time for modeling a galactic system with a SMBH in the
quasi-static limit. This model is applicable to systems either out of their
accretion-phase at late times or either for those undergoing into a very slow
accretion-phase, such as some early-type giant elliptic galaxies and bulges.
  On the other hand, very recent direct observation of Sagittarius A by the
Event Horizon Telescope will open an era of explorations of the deep-inner
galactic region of the Milky Way that will enable us to test and distinguish
various dark matter models. Thus we use our model to give a very first step
towards that direction. We derive the stellar kinematics induced by this sort
dark matter to obtain information of the black hole's influence into the
observable features of the velocity field of visible matter deep inside the
galaxy. Thus we compute the radial velocity, acceleration and velocity
dispersion densities for some realistic cases.
