Galaxy rotation curves in modified gravity models
In this work, we investigate the possibility that the galaxy rotation curves can be explained in the framework of modified gravity models that introduce a Yukawa term in the gravitational potential. We include dark matter and assume that the fifth-force couples differently to dark matter and to bary...
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| Main Authors: | , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
10 August 2018
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| In: |
Journal of cosmology and astroparticle physics
Year: 2018, Issue: 8 |
| ISSN: | 1475-7516 |
| DOI: | 10.1088/1475-7516/2018/08/012 |
| Online Access: | Verlag, Volltext: http://dx.doi.org/10.1088/1475-7516/2018/08/012 Verlag, Volltext: http://stacks.iop.org/1475-7516/2018/i=08/a=012 
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| Author Notes: | Álefe de Almeida, Luca Amendola and Viviana Niro |
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| 245 | 1 | 0 | |a Galaxy rotation curves in modified gravity models |c Álefe de Almeida, Luca Amendola and Viviana Niro |
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| 520 | |a In this work, we investigate the possibility that the galaxy rotation curves can be explained in the framework of modified gravity models that introduce a Yukawa term in the gravitational potential. We include dark matter and assume that the fifth-force couples differently to dark matter and to baryons. We aim at constraining the modified gravity parameters β and λ, that is, the strength and the range of the Yukawa fifth force, respectively, using a set of 40 galaxy rotation curves data from the SPARC catalogue. We include baryonic gas, disk and bulge components, along with a NFW halo of dark matter. Each galaxy rotation curve is modeled with three free parameters, beside the two global Yukawa parameter. We find that the inclusion of the Yukawa term improves the χ 2 from 680.75 to 536.23 for 655 degrees of freedom. As global best-fit we obtain β = 0.34±0.04 and λ = 5.61±0.91kpc and a dark matter content on average 20% smaller than without the Yukawa term. The Bayesian evidence in favor of a NFW profile plus Yukawa term is higher than 8σ with respect to the standard gravity parametrization. | ||
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