# Axisymmetric Schwarzschild models of an isothermal axisymmetric mock dwarf spheroidal galaxy

## TL;DR

This study evaluates Schwarzschild's orbit superposition method for modeling flattened dwarf spheroidal galaxies, demonstrating it can reliably measure mass and scale parameters even with limited data, but struggles to constrain flattening.

## Contribution

The paper introduces an application of Schwarzschild modeling to flattened dwarf spheroidal galaxies, assessing its effectiveness in determining key parameters with mock data.

## Key findings

- Mass and scale radius can be accurately constrained.
- Flattening parameter remains largely unconstrained.
- Reliable mass estimates are possible with ~2000 velocities.

## Abstract

We test the ability of Schwarzschild's orbit superposition method in measuring the mass content, scale radius and shape of a flattened dwarf spheroidal galaxy. Until now, most dynamical model efforts have assumed that dwarf spheroidal galaxies and their host halos are spherical. We use an Evans model (1993) to construct an isothermal mock galaxy whose properties somewhat resemble those of the Sculptor dwarf spheroidal galaxy. This mock galaxy contains flattened luminous and dark matter components, resulting in a logarithmic profile for the global potential. We have tested how well our Schwarzschild method could constrain the characteristic parameters of the system for different sample sizes, and also if the functional form of the potential was unknown. When assuming the true functional form of the potential, the Schwarzschild modelling technique is able to provide an accurate and precise measurement of the characteristic mass parameter of the system and reproduces well the light distribution and the stellar kinematics of our mock galaxy. When assuming a different functional form for the potential, such as a flattened NFW profile, we also constrain the mass and scale radius to their expected values. However in both cases, we find that the flattening parameter remains largely unconstrained. This is likely because the information content of the velocity dispersion on the geometric shape of the potential is too small, since $\sigma$ is constant across our mock dSph. Our results using Schwarzschild's method indicate that the mass enclosed can be derived reliably, even if the flattening parameter is unknown, and already for samples containing 2000 line-of-sight radial velocities, such as those currently available. Further applications of the method to more general distribution functions of flattened systems are needed to establish how well the flattening of dSph dark halos can be determined.