# A study of stellar orbit fractions: simulated IllustrisTNG galaxies compared to CALIFA observations

## TL;DR

This study compares stellar orbit fractions in simulated IllustrisTNG galaxies with CALIFA observations, finding broad agreement in mass dependencies and specific features, while noting some discrepancies likely due to heating mechanisms.

## Contribution

It provides a detailed comparison of stellar orbit compositions between simulations and observations, highlighting areas of agreement and discrepancy in galaxy kinematic properties.

## Key findings

- Broad reproduction of observed orbit fractions by TNG100
- Peak and trough features at 1-2E10 solar masses are matched
- Some systematic differences in cold-orbit fractions and scatter

## Abstract

Motivated by the recently discovered kinematic "Hubble sequence" shown by the stellar orbit-circularity distribution of 260 CALIFA galaxies, we make use of a comparable galaxy sample at z = 0 with a stellar mass range from 5E9 to 5E11 solar masses, selected from the IllustrisTNG simulation and study their stellar orbit compositions in relation to a number of other fundamental galaxy properties.We find that the TNG100 simulation broadly reproduces the observed fractions of different orbital components and their stellar mass dependencies. In particular, the mean mass dependencies of the luminosity fractions for the kinematically warm and hot orbits are well reproduced within model uncertainties of the observed galaxies. The simulation also largely reproduces the observed peak and trough features at a stellar mass of 1-2E10 solar masses, in the mean distributions of the cold- and hot-orbit fractions, respectively, indicating fewer cooler orbits and more hotter orbits in both more- and less-massive galaxies beyond such a mass range. Several marginal disagreements are seen between the simulation and observations: the average cold-orbit (counter-rotating) fractions of the simulated galaxies below (above) a stellar mass of 6E10 solar masses, are systematically higher than the observational data by < 10% (absolute orbital fraction); the simulation also seems to produce more scatter for the cold-orbit fraction and less so for the non-cold orbits at any given galaxy mass. Possible causes that stem from the adopted heating mechanisms are discussed.