  In the first part of this article we expand three fundamental aspects of the
methodology connected to the determination of a relation among the spatial
density and the gravitational potential that can be specialised to distinct
mass density agglomerations. As a consequence, we obtain general relations for
the diagonal entries of a square symmetric matrix without zeros, we provide an
expression of the gravitational potential, suitable, to represent several
different mass density configurations, and we determine relations for the
semi-axes of a triaxial spheroidal mass distribution, as a function of the
spheroid mass density, volume density and radius. In the second part of this
manuscript, we employ the tools developed in the first part, to analyse the
mass density content and the inner and global structure of the dark matter
haloes of UGC 8490 and UGC 9753, through the fits to the dark matter rotation
curves of the two galaxies, assuming a triaxial spheroidal dark matter mass
configuration. We employ the Navarro Frenk and White, Burkert, DiCintio,
Einasto and Stadel dark matter models, and we obtain that both a cored Burkert
and cuspy DiCintio and Navarro Frenk and White inward dark matter distributions
could represent equally well the observed data, furthermore we determine an
oblate spheroidal dark matter mass density configuration for UGC 8490 and UGC
9753. The latter outcome is confirmed by the estimation of the gravitational
torques exerted by the dark matter halo of each analysed galaxy, on the
corresponding baryonic components.
