# Non-sphericity of ultralight axion dark matter haloes in the Galactic dwarf spheroidal galaxies

## TL;DR

This study uses non-spherical models to analyze dwarf spheroidal galaxies, providing more realistic constraints on ultralight axion dark matter and revealing a preference for flattened dark matter halos, challenging previous spherical assumptions.

## Contribution

It introduces non-spherical dynamical models for dwarf spheroidals to better constrain ultralight axion dark matter properties, highlighting the importance of halo shape considerations.

## Key findings

- dSphs prefer flattened dark matter halos
- Constraints on ULA mass are less stringent with non-spherical models
- Dark matter halos are more elongated than numerical predictions

## Abstract

Ultralight-axion (ULA) dark matter is one of the possible solutions to resolve small-scale problems, especially the core-cusp problem. This is because ULA dark matter can create a central soliton core in all dark matter haloes stemmed from the quantum pressure against gravity below the de Broglie wavelength, which becomes manifest on astrophysical scales with axion mass range $\sim10^{-22}$ eV. In this work, we apply our non-spherical dynamical models to the kinematic data of eight classical dwarf spheroidals (dSphs) to obtain more reliable and realistic limits on ULA particle mass. This is motivated by the reasons that the light distributions of the dSphs are not spherical, nor are the shapes of dark matter haloes predicted by ULA dark matter simulations. Compared with the previous studies on ULA dark matter assuming spherical mass models, our result is less stringent than those constraints due to the uncertainties on non-sphericity. On the other hand, remarkably, we find that the dSphs would prefer to have a flattened dark matter halo rather than a spherical one, especially Draco favours a strongly elongated dark matter halo caused naively by the assumption of a soliton-core profile. Moreover, our consequent non-spherical core profiles are much more flattened than numerical predictions based on ULA dark matter, even though there are still uncertainties on the estimation of dark matter halo structure. To alleviate this discrepancy, further understanding of baryonic and/or ULA dark matter physics on small mass scales might be needed.