Testing Scalar Field Dark Matter models in M31 galaxy through the Rotation Curve analysis

TL;DR

This study assesses scalar field dark matter models against M31's rotation curve, finding that cored halos like FDM best fit the galaxy's kinematic data, especially with a two-bulge baryonic structure.

Contribution

It compares three scalar field dark matter models using detailed rotation curve analysis and Bayesian criteria, highlighting the effectiveness of FDM in explaining M31's dynamics.

Findings

Two-bulge baryonic model improves fit quality.

FDM provides the most consistent scalar field dark matter description.

Smooth cored halos outperform other models in fitting M31 data.

Abstract

We explore the viability of scalar field dark matter halo models through the rotation curve analysis of the Andromeda galaxy (M31), taking into account a realistic description of its baryonic structure. The mass model includes a stellar disk described by the Freeman profile and two alternative bulge configurations: a classical single de Vaucouleurs bulge and a two-component structure consisting of inner and main bulges modeled by exponential sphere profiles. The dark matter halo is modeled using three scalar field motivated models: fuzzy dark matter (FDM), Bose-Einstein condensate and multistate scalar-field dark matter. The model parameters are determined through the Levenberg-Marquardt nonlinear least-squares fitting, and the relative performance of the models is evaluated using the Bayesian Information Criterion which allows a direct comparison with previous phenomenological halo studies performed for the same galaxy. We find that the two-bulge baryonic configuration ensures a better statistical description of the M31 rotation curve, independently of the adopted halo model. The results also suggest that, within scalar field dark matter scenarios, smooth cored halos, such as FDM, provide the most consistent description of the M31 kinematics.