Abstract
In this work we investigate the behaviour of SFDM at small scales, specifically its viability in reproducing galactic rotation curves. We consider a scalar field with no selfinteraction. In this case, the only free parameter is the mass of the scalar field. By fitting the galactic rotational curves it is found the allowed region for the mass of the scalar field. We discuss those limits with previous bounds on the mass coming from astrophysical considerations. The galactic density profiles within the SFDM is found by solving a non linear system of ordinary differential equations for the scalar and the gravitational fields. Given the appropriate boundary conditions, the system becomes an eigenvalue problem which is solved by an inner- outer interaction using an efficient computational method. This method is faster than the predecessors, and could be implemented in parallel computing.
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