Ultra-Light Dark Matter in Ultra-Faint Dwarf Galaxies

TL;DR

This paper investigates ultra-light scalar field dark matter as a solution to small-scale galactic structure issues, using new dwarf galaxy data to estimate the particle mass and support the wave dark matter model.

Contribution

It provides observational constraints on ultra-light dark matter particle mass using ultra-faint dwarf galaxy measurements, supporting the wave dark matter scenario.

Findings

Estimated dark matter particle mass: 3.7-5.6×10^{-22} eV.

Supports formation of solitonic cores in dwarf galaxies.

Aligns with observations of cored density profiles.

Abstract

Cold Dark Matter (CDM) models struggle to match the observations at galactic scales. The tension can be reduced either by dramatic baryonic feedback effects or by modifying the particle physics of CDM. Here, we consider an ultra-light scalar field DM particle manifesting a wave nature below a DM particle mass-dependent Jeans scale. For DM mass $m\sim10^{-22}{\rm eV}$, this scenario delays galaxy formation and avoids cusps in the center of the dark matter haloes. We use new measurements of half-light mass in ultra-faint dwarf galaxies Draco II and Triangulum II to estimate the mass of the DM particle in this model. We find that if the stellar populations are within the core of the density profile then the data are in agreement with a wave dark matter model having a DM particle with $m\sim 3.7-5.6\times 10^{-22}{\rm eV}$. The presence of this extremely light particle will contribute to the formation of a central solitonic core replacing the cusp of a Navarro-Frenk-White profile and bringing predictions closer to observations of cored central density in dwarf galaxies.