N-body self-consistent stars-halo modeling of the Fornax dwarf galaxy
  We present nearly self-consistent stellar-halo models of the Fornax dwarf
spheroidal galaxy associated with the Milky Way galaxy. Such galaxies are
dominated by dark matter and have almost no gas in the system. Therefore, they
are excellent objects for N-body modeling that takes into account visible and
dark matter halo components. In order to model the dark matter halo inferred
from the analysis of the measured velocities of Fornax's stars, we constructed
several self-consistent quasi-equilibrium models based on two source code sets.
One of them (GalactICS Software, NEMO) deals with the self-consistent
distribution function modeling which depends on energy $E$ and vertical
component of the angular momentum $L_z$. The other is included in the AGAMA
framework and is based on Schwarzschild's calculation of orbits. It can
reproduce the non-spherical self-consistent structure of Fornax as the weighted
sum of orbit contributions to the galactic density even though the inferred
dark halo parameters come from Jeans analysis which does not require that any
distribution functions should be positive. To guess the parameters which make
the N-body models close to the visible object we use the stellar-dark matter
model of the Fornax galaxy based on hydrodynamic axisymmetric Jeans equations
taking into account the velocity anisotropy parameter. Then we studied the
evolution of the models by performing N-body simulations with the falcON code
in order to test their stability. The variability of the model parameters over
time was obtained during simulations. The AGAMA models show the best agreement
of the resulting velocity dispersion profiles with the observed data.
