Kinematic signatures of impulsive supernova feedback in dwarf galaxies

TL;DR

This paper investigates how impulsive supernova feedback creates distinct phase space features in dwarf galaxies, providing a potential observational test to distinguish it from dark matter models like SIDM.

Contribution

It predicts specific phase space signatures resulting from supernova feedback, offering a new way to test the dominant core formation mechanism in dwarf galaxies.

Findings

Overdense star groups with similar ages and metallicities form shells in phase space due to supernova feedback.

Presence of these features indicates supernova-driven core formation, absence suggests alternative dark matter models.

Provides a method to differentiate between supernova feedback and SIDM in dwarf galaxy evolution.

Abstract

Impulsive supernova feedback and non-standard dark matter models, such as self-interacting dark matter (SIDM), are the two main contenders for the role of the dominant core formation mechanism at the dwarf galaxy scale. Here we show that the impulsive supernova cycles that follow episodes of bursty star formation leave distinct features in the distribution function of stars: groups of stars with similar ages and metallicities develop overdense shells in phase space. If cores are formed through supernova feedback, we predict the presence of such features in star-forming dwarf galaxies with cored host halos. Their systematic absence would favor alternative dark matter models, such as SIDM, as the dominant core formation mechanism.