  In our previous work we confirmed the reliability of the spherically
symmetric Schwarzschild orbit-superposition method to recover the mass and
velocity anisotropy profiles of spherical dwarf galaxies. Here we investigate
the effect of its application to intrinsically non-spherical objects. For this
purpose we use a model of a dwarf spheroidal galaxy formed in a numerical
simulation of a major merger of two disky dwarfs. The shape of the stellar
component of the merger remnant is axisymmetric and prolate which allows us to
identify and measure the bias caused by observing the spheroidal galaxy along
different directions, especially the longest and shortest principal axis. The
modelling is based on mock data generated from the remnant that are
observationally available for dwarfs: projected positions and line-of-sight
velocities of the stars. In order to obtain a reliable tool while keeping the
number of parameters low we parametrize the total mass distribution as a
radius-dependent mass-to-light ratio with just two free parameters we aim to
constrain. Our study shows that if the total density profile is known, the
true, radially increasing anisotropy profile can be well recovered for the
observations along the longest axis whereas the data along the shortest axis
lead to the inference an incorrect, isotropic model. On the other hand, if the
density profile is derived from the method as well, the anisotropy is always
underestimated but the total mass profile is well recovered for the data along
the shortest axis whereas for the longest axis the mass content is
overestimated.
