# Evaluating the ability of triaxial Schwarzschild modelling to estimate properties of galaxies from the Illustris simulation

## TL;DR

This study assesses the effectiveness of Schwarzschild's orbit-superposition method in accurately estimating galaxy properties from high-resolution simulated data, finding it reliably recovers mass profiles and orbital distributions with some biases.

## Contribution

It provides a comprehensive evaluation of Schwarzschild modelling on simulated galaxies, highlighting its strengths and limitations in recovering galaxy properties.

## Key findings

- Total mass within effective radius is recovered within ±15%.
- Stellar mass is underestimated by ~24%, dark matter overestimated by ~38%.
- Velocity anisotropy and orbital distributions are well reconstructed.

## Abstract

We evaluate the capabilities of Schwarzschild's orbit-superposition method by applying it to galaxies from the large scale, high resolution Illustris simulation. Nine early-type galaxies with a range of triaxiality are selected, and we create mock integral field unit data for five line-of-sight projections of each galaxy. Each of the 45 mock data sets is taken as an independent observed galaxy. Using van den Bosch's 2008 triaxial Schwarzschild implementation, we assess model estimates of various galaxy properties, covering mass profiles, intrinsic shapes, stellar orbit distributions and velocity anisotropies. Total mass within $\overline{R_{\rm e}}$ is recovered well with average deviations within $\pm15$ percent. Stellar mass is underestimated by $\sim24$ percent and dark matter overestimated by $\sim38$ percent (assuming an NFW dark matter profile and allowing for degeneracy between stellar mass and dark matter mass). Using a gNFW profile, these values improve to $\sim13$ percent for stellar mass and $\sim18$ percent for dark matter. Axis ratio estimates show a moderate bias of $\Delta (b/a)=0.07$ and $\Delta (c/a)=0.14$ ($a\ge b\ge c$). Distributions of the orbit circularities $\lambda_z$ and $\lambda_x$, representing rotation about the minor and major axes, are well reconstructed. Separating orbits into thermal categories, our models match the average fractions of these categories to within $10$ percent. Velocity anisotropy is well estimated with values matching in the inner regions but becoming slightly radially biased in the outer regions. Overall, the galaxy property estimates we obtained using Schwarzschild modelling are not implausible and are representative of the simulated galaxies we modelled.