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Advances in High Energy Physics
Volume 2017 (2017), Article ID 4025386, 14 pages
Research Article

Bose-Einstein Condensate Dark Matter Halos Confronted with Galactic Rotation Curves

Institute of Physics, University of Szeged, Dóm Tér 9, Szeged 6720, Hungary

Correspondence should be addressed to L. Á. Gergely; moc.liamg@ylegreg.a.olzsal

Received 7 October 2016; Revised 15 December 2016; Accepted 25 December 2016; Published 8 February 2017

Academic Editor: Sergei D. Odintsov

Copyright © 2017 M. Dwornik et al. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP3.


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.