Bose-Einstein Condensate Dark Matter Halos confronted with galactic rotation curves

TL;DR

This study compares Bose-Einstein Condensate and NFW dark matter halo models against galactic rotation curves, finding BEC fits dwarf galaxies better, while NFW performs better for larger galaxies, highlighting their respective strengths and limitations.

Contribution

It provides a comparative analysis of BEC and NFW dark matter models across different galaxy types using observational rotation curve data.

Findings

BEC model fits dwarf galaxy rotation curves better.

NFW model fits larger galaxy rotation curves better.

Both models obey the Tully-Fisher relation with characteristic parameter relations.

Abstract

We present a comparative confrontation of both the Bose-Einstein Condensate (BEC) and the Navarro-Frenk-White (NFW) dark halo models with galactic rotation curves. We employ 6 High Surface Brightness (HSB), 6 Low Surface Brightness (LSB), and 7 dwarf galaxies with rotation curves falling into two classes. In the first class rotational velocities increase with radius over the observed range.The BEC and NFW models give comparable fits for HSB and LSB galaxies of this type, while for dwarf galaxies the fit is significantly better with the BEC model. In the second class the rotational velocity of HSB and LSB galaxies exhibits long flat plateaus, resulting in better fit with the NFW model for HSB galaxies and comparable fits for LSB galaxies. We conclude that due to its central density cusp avoidance the BEC model fits better dwarf galaxy dark matter distribution. Nevertheless it suffers from sharp cutoff in larger galaxies, where the NFW model performs better. The investigated galaxy sample obeys the Tully-Fisher relation, including the particular characteristics exhibited by dwarf galaxies. In both models the fitting enforces a relation between dark matter parameters: the characteristic density and the corresponding characteristic distance scale with an inverse power.