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In our previous work we confirmed the reliability of the sphericallysymmetric Schwarzschild orbit-superposition method to recover the mass andvelocity anisotropy profiles of spherical dwarf galaxies. Here we investigatethe effect of its application to intrinsically non-spherical objects. For thispurpose we use a model of a dwarf spheroidal galaxy formed in a numericalsimulation of a major merger of two disky dwarfs. The shape of the stellarcomponent of the merger remnant is axisymmetric and prolate which allows us toidentify and measure the bias caused by observing the spheroidal galaxy alongdifferent directions, especially the longest and shortest principal axis. Themodelling is based on mock data generated from the remnant that areobservationally available for dwarfs: projected positions and line-of-sightvelocities of the stars. In order to obtain a reliable tool while keeping thenumber of parameters low we parametrize the total mass distribution as aradius-dependent mass-to-light ratio with just two free parameters we aim toconstrain. Our study shows that if the total density profile is known, thetrue, radially increasing anisotropy profile can be well recovered for theobservations along the longest axis whereas the data along the shortest axislead to the inference an incorrect, isotropic model. On the other hand, if thedensity profile is derived from the method as well, the anisotropy is alwaysunderestimated but the total mass profile is well recovered for the data alongthe shortest axis whereas for the longest axis the mass content isoverestimated.

The effect of non-sphericity on mass and anisotropy measurements in dSph galaxies with Schwarzschild method