Dynamical reconstruction of SPARC galactic halos within self-interacting fuzzy dark matter

TL;DR

This paper demonstrates that self-interacting fuzzy dark matter can fit galaxy rotation data and reconstruct galactic halos dynamically, providing a new approach to understanding dark matter distribution in galaxies.

Contribution

It introduces a method to fit galaxy data with self-interacting fuzzy dark matter and reconstructs galactic halos dynamically using numerical simulations.

Findings

Fuzzy dark matter with self-interaction fits 17 galaxy rotation curves.

Identifies specific boson mass and self-coupling parameters.

Demonstrates viable halo reconstructions over billion-year timescales.

Abstract

Fuzzy Dark Matter with non-zero quartic self-interaction (SFDM) is shown to be a viable model for simultaneously fitting 17 dark-matter-dominated galaxies from the SPARC database with a single $(m,g)$ point in the space of boson masses and self-coupling constants: $\log_{10}\left(m \,[\mathrm{eV}/c^2] \right) = \log_{10}(1.98)-22^{+0.8}_{-0.6}$ and $\log_{10}\left(g \, [\mathrm{eV \, m}^3/kg] \right) = \log_{10}(9.08)-10^{+0.4}_{-1.2}$. This is based on the combination of an appropriately constructed static super-Gaussian profile for the inner galactic core (`soliton') region, and a Navarro-Frenk-White profile for the surrounding halo region. The explicit identification of a non-zero interaction strength may resolve issues of inconsistent constraints in non-interacting FDM. Our identification of these parameters enables the explicit {\em dynamical} reconstruction of potential host halos for such galaxies through numerical solution of the SFDM equations; we outline a {proof-of-principle procedure via merger simulations} for two galaxies (UGCA444, UGC07866), and show that this yields viable rotation curves over a dynamical period of ${\cal O}(1) \, Gyr$.