Distribution functions for the modelling of accretion remnants in Milky Way-like galaxies: insights from IllustrisTNG

TL;DR

This study evaluates how well various distribution functions model the phase-space distributions of accretion remnants in Milky Way-like galaxies using IllustrisTNG simulations, providing insights into their equilibrium states and kinematic properties.

Contribution

It demonstrates the effectiveness of different distribution function models in describing the kinematics of merger remnants, especially high-anisotropy cases like Gaia-Sausage/Enceladus.

Findings

Distribution functions fit well to energy and angular momentum distributions.

Remnants with high anisotropy are better modeled with superpositions of two Osipkov-Merritt DFs.

Osipkov-Merritt profile with scale radius 2-4 kpc effectively models Gaia-Sausage/Enceladus.

Abstract

We study accretion remnants around Milky Way analogs in the IllustrisTNG simulations to determine how well commonly used distribution functions (DFs) describe their phase-space distributions. We identify 30 Milky Way analogs and 116 remnants from mergers with stellar mass ratios greater than 1:20. Two-power density profiles, as well as rotating constant-anisotropy and Osipkov-Merritt DFs are fit to the remnants. We determine that the remnants are suitable for equilibrium modelling by assessing them in the context of the Jeans equation. Each of the models we consider are reasonably able to fit the stellar remnant energy and angular momentum distribution, as well as the magnitude and shape of velocity dispersion profiles. Case studies matched to two well-known merger remnants in the stellar halo-Gaia-Sausage/Enceladus (GS/E) and Sequoia-are explored in more depth. We find good evidence that remnants with high anisotropy $\beta$, such as GS/E, are better modelled with a superposition of two Osipkov-Merritt DFs than either a constant-anisotropy model or a single Osipkov-Merritt DF. We estimate an Osipkov-Merritt profile with scale radius between 2-4 kpc would be a good first-order representation of GS/E, and comment on existing observational evidence for this as well as studies which could demonstrate it. Overall, we find that DF-based models work well for describing the kinematics of large merger remnants. Our results will be an important reference for future studies which seek to constrain both the spatial and kinematic properties of merger remnants in the Milky Way stellar halo.