Impulsive mixing of stellar populations in dwarf spheroidal galaxies

TL;DR

This study investigates how stellar populations in dwarf spheroidal galaxies respond to sudden and gradual changes in dark matter potential, revealing effects on size, velocity, and mixing of populations, with implications for galaxy mass estimates.

Contribution

It provides a detailed analysis of stellar response to dark matter potential changes, highlighting differences between impulsive and adiabatic regimes and their impact on galaxy properties.

Findings

Half-light radii expand and velocity dispersions decrease with dark matter removal.

Metallicity gradients flatten as dark matter is slowly removed.

Impulsive perturbations cause stellar populations to develop power-law density tails and mix energetically.

Abstract

We study the response of mono-energetic stellar populations with initially isotropic kinematics to impulsive and adiabatic changes to an underlying dark matter potential. Half-light radii expand and velocity dispersions decrease as enclosed dark matter is removed. The details of this expansion and cooling depend on the time scale on which the underlying potential changes. In the adiabatic regime, the product of half-light radius and average velocity dispersion is conserved. We show that the stellar populations maintain centrally isotropic kinematics throughout their adiabatic evolution, and their densities can be approximated by a family of analytical radial profiles. Metallicity gradients within the galaxy flatten as dark matter is slowly removed. In the case of strong impulsive perturbations, stellar populations develop power-law-like density tails with radially biased kinematics. We show that the distribution of stellar binding energies within the dark matter halo substantially widens after an impulsive perturbation, no matter the sign of the perturbation. This allows initially energetically separated stellar populations to mix, to the extent that previously chemo-dynamically distinct populations may masquerade as a single population with large metallicity and energy spread. Finally, we show that in response to an impulsive perturbation, stellar populations that are deeply embedded in cored dark matter halos undergo a series of damped oscillations before reaching a virialised equilibrium state, driven by inefficient phase mixing in the harmonic potentials of cored halos. This slow return to equilibrium adds substantial systematic uncertainty to dynamical masses estimated from Jeans modeling or the virial theorem.