Dark matter profiles of SPARC galaxies: a challenge to fuzzy dark matter

Abstract

Stellar and gas kinematics of galaxies are a sensitive probe of the dark matter distribution in the halo. The popular fuzzy dark matter models predict the peculiar shape of density distribution in galaxies: specific dense core with sharp transition to the halo. Moreover, fuzzy dark matter predicts scaling relations between the dark matter particle mass and density parameters. In this work, we use a Bayesian framework and several dark matter halo models to analyse the stellar kinematics of galaxies using the Spitzer Photometry & Accurate Rotation Curves database. We then employ a Bayesian model comparison to select the best halo density model. We find that more than half of the galaxies prefer the fuzzy dark model against standard dark matter profiles (NFW, Burkert, and cored NFW). While this seems like a success for fuzzy dark matter, we also find that there is no single value for the particle mass that provides a good fit for all galaxies.

ULDM self-interactions, tidal effects and tunnelling out of satellite galaxies

“…However in recent years, much of the relevant mass range for ULDM with no self-interactions 10 −24 eV, 10 −20 eV has been severely constrained using various astrophysical and cosmological observations. See for instance constraints from rotation curves [44][45][46], Lyman-α data [47][48][49], CMB and Large Scale Structure [50,51], dynamical heating of stars in ultra-faint dwarf galaxies [52], as well as recent results from NANOGrav and Pulsar Timing Arrays [8,53].…”

Phenomenology of wavelike vector dark matter nonminimally coupled to gravity

“…In this paper, we study wavelike VDM that is nonminimally coupled to gravity in the wave regime, where the mass of DM particles is m 30eV. Although the DM mass m ∼ 10 −22 eV is preferred in some galaxies [71][72][73], a lower bound m 10 −19 eV has been reported by constraining velocity dispersion in Segue 1 and Segue 2 galaxies [74], and it further increases to m 10 −18 eV if the DM is produced after inflation via a process with a finite-correlation length [75]. The impact of nonminimal couplings on these constraints warrants a detailed analysis, and for generality we focus on m 10 −22 eV.…”