Scalar field dark matter mass model and evolution of rotation curves for low surface brightness galaxies

• Published in: Monthly notices of the Royal Astronomical Society Vol. 444; no. 1; pp. 185 - 191
• Main Authors: Martinez-Medina, L. A., Matos, T.
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 11-10-2014
• Subjects: Astronomy; Dark matter; Simulation; Star & galaxy formation; hydrodynamics; methods: numerical; dark matter; galaxies: haloes
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stu1453

We study the evolution of gas rotation curves within the scalar field dark matter (SFDM) model. In this model, the galactic haloes are astronomical Bose–Einstein condensate drops of scalar field (SF). These haloes are characterized by a constant density core and are consistent with observed rotation curves of dark matter (DM) dominated galaxies, a missing feature in cold dark matter haloes resulting from DM-only simulations. We add the baryonic component to the SFDM haloes and simulate the evolution of the DM tracer in a set of grid-based hydrodynamic simulations aimed to analyse the evolution of the rotation curves and the gas density distribution in the case of DM dominated galaxies. Previous works had found that when considering an exact analytic solution for a static SF configuration, the free parameters of the model allow for good fits to the rotation curves, we confirm that in our simulations but now taking into account the evolution of the baryonic component in a static DM and stellar disc potential. Including live gas is a step forward from the previous work using SFDM, as for example, the rotation velocity of the gas is not always exactly equal to the circular velocity of a test particle on a circular orbit. Contrasting with the data the cored mass model presented here is preferred instead of a cuspy one.