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We model mock observations of collisionless  N ‐body disc–disc mergers with the same axisymmetric orbit superposition program that has been used to model elliptical galaxies in Coma. The remnants sample representatively the shape distribution of disc–disc mergers, including the most extreme cases, like highly prolate, maximally triaxial and dominantly oblate objects. The aim of our study is to better understand how the assumption of axial symmetry affects reconstructed masses and stellar motions of systems which are intrinsically not axisymmetric, whether the axisymmetry assumption then leads to a bias and how such a potential bias can be recognized in models of real galaxies. The mass recovery at the half‐light radius depends on viewing angle and intrinsic shape: edge‐on views allow to reconstruct total masses with an accuracy between 20 per cent (triaxial/prolate remnants) and 3 per cent (oblate remnant). Masses of highly flattened, face‐on systems are underestimated by up to 50 per cent. Deviations in local mass densities can be larger where remnants are strongly triaxial or prolate. Luminous mass‐to‐light ratios are sensitive to box orbits in the remnants. Box orbits cause the central value of the Gauss–Hermite parameter  H  4  to vary with viewing angle. Reconstructed luminous mass‐to‐light ratios, as well as reconstructed central masses, follow this variation. Luminous mass‐to‐light ratios are always underestimated (up to a factor of 2.5). Respective dark haloes in the models can be overestimated by about the same amount, depending again on viewing angle. Reconstructed velocity anisotropies β depend on viewing angle as well as on the orbital composition of the remnant and are mostly accurate to about  Δβ= 0.2 . Larger deviations can occur towards the centre or the outer regions, respectively. We construct  N ‐body realizations of the Schwarzschild models to discuss chaotic orbits and the virial equilibrium in our models. In this study we explore the extreme limits of axisymmetric models. Apparently flattened, rotating ellipticals of intermediate mass are likely close to both, axial symmetry and edge‐on orientation. Our results imply that Schwarzschild models allow a reconstruction of their masses and stellar anisotropies with high accuracy.

Axisymmetric orbit models of N ‐body merger remnants: a dependency of reconstructed mass on viewing angle