Testing Bose–Einstein condensate dark matter models with the SPARC galactic rotation curves data

Abstract

The nature of one of the fundamental components of the Universe, dark matter, is still unknown. One interesting possibility is that dark matter could exist in the form of a self-interacting Bose–Einstein Condensate (BEC). The fundamental properties of dark matter in this model are determined by two parameters only, the mass and the scattering length of the particle. In the present study we investigate the properties of the galactic rotation curves in the BEC dark matter model, with quadratic self-interaction, by using 173 galaxies from the recently published Spitzer Photomery & Accurate Rotation Curves (SPARC) data. We fit the theoretical predictions of the rotation curves in the slowly rotating BEC models with the SPARC data by using genetic algorithms. We provide an extensive set of figures of the rotation curves, and we obtain estimates of the relevant astrophysical parameters of the BEC dark matter halos (central density, angular velocity and static radius). The density profiles of the dark matter distribution are also obtained. It turns out that the BEC model gives a good description of the SPARC data. The presence of the condensate dark matter could also provide a solution for the core–cusp problem.

Phases of the Bose–Einstein Condensate Dark Matter Model with Both Two- and Three-Particle Interactions

“…At the same time, the best fitted dependencies, represented by other curves, always require Q > 0. This implies that the repulsive pair interaction should be taken into account in realistic models of dark matter in (dwarf) galaxies [11,20].…”

“…Positions of the BEC model of DM were especially enforced after the works [7][8][9] which demonstrated the ability of BEC DM to avoid the core-cusp and gravitational collapse [10] problems. Furthermore, the model gives a quite successful description [7,[11][12][13] of the rotation curves of a number of galaxies-at least the dwarf and low surface brightness ones.…”

Phases of the Bose-Einstein condensate dark matter model with both two- and three-particle interactions

“…Positions of BEC model of DM were especially enforced after the works [7,8,9] which demonstrated ability of BEC DM to avoid the core-cusp and the gravitational collapse [10] problems. Also, the model gives quite successful description [7,11,12,13] of the rotation curves of a number of galaxies, at least dwarf and the low surface brightness ones.…”

Static spherically symmetric three-form stars

“…The equation of state of the condensate is characterized by two important physical parameters, the mass of the condensate particle m, and the scattering length a [71]. For a condensate with quartic non-linearity, the equation of state is polytropic with index n = 1, and it is given by p(ρ) = Kρ 2 [71][72][73]. In the case of a neutron condensate…”