  Rotating bosonic dark matter halos are considered as potential candidates for
modeling dark matter in galactic halos. These bosonic dark matter halos can be
viewed as a dilute and very extended version of bosonic stars, and the methods
used for the calculation and analysis of the latter objects can be directly
applied. Bosonic stars, a hypothetical type of astrophysical objects, are
categorized into two primary families, based on the nature of the particles
composing them: Einstein-Klein-Gordon stars and Proca stars. We examine various
models from both families and the rotation curves which their contribution
induces in different galaxies, to identify the most plausible candidates that
explain the flattening of orbital velocities observed in galactic halos. By
exploring different combinations of our dark matter models with observable
galactic features, we propose an interesting source to compensate for the
apparent lack of matter in dwarf and spiral galaxies, providing a possible
explanation for this longstanding astronomical puzzle.
