  Popular models for describing the luminosity-density profiles of dynamically
hot stellar systems (e.g., Jaffe, Hernquist, Dehnen) were constructed to match
the deprojected form of de Vaucouleurs' $R^{1/4}$ light-profile. However, we
now know that elliptical galaxies and bulges display a mass-dependent range of
structural profiles. To compensate this, the model in Terzic & Graham was
designed to closely match the deprojected form of Sersic $R^{1/n}$
light-profiles, including deprojected exponential light-profiles and galaxies
with partially depleted cores. It is thus applicable for describing bulges in
spiral galaxies, dwarf elliptical galaxies, both ``power-law'' and ``core''
elliptical galaxies, also dark matter halos formed from $\Lambda$CDM
cosmological simulations.
  In this paper, we present a new family of triaxial density-potential-force
triplets, which generalizes the spherical model reported in Terzic & Graham to
three dimensions. If the (optional) power-law core is present, it is a
5-parameter family, while in the absence of the core it reduces to 3
parameters. The isodensity contours in the new family are stratified on
confocal ellipsoids and the potential and forces are expressed in terms of
integrals which are easy to evaluate numerically. We provide the community with
a suite of numerical routines for orbit integration, which feature: optimized
computations of potential and forces for this family; the ability to run
simulations on parallel platforms; and modular and easily editable design.
