Scalar Field (Wave) Dark Matter
  Recent high-quality observations of dwarf and low surface brightness (LSB)
galaxies have shown that their dark matter (DM) halos prefer flat central
density profiles. On the other hand the standard cold dark matter model
simulations predict a more cuspy behavior. Feedback from star formation has
been widely used to reconcile simulations with observations, this might be
successful in field dwarf galaxies but its success in low mass galaxies remains
uncertain. One model that have received much attention is the scalar field dark
matter model. Here the dark matter is a self-interacting ultra light scalar
field that forms a cosmological Bose-Einstein condensate, a mass of
$10^{-22}$eV/c$^2$ is consistent with flat density profiles in the centers of
dwarf spheroidal galaxies, reduces the abundance of small halos, might account
for the rotation curves even to large radii in spiral galaxies and has an early
galaxy formation. The next generation of telescopes will provide better
constraints to the model that will help to distinguish this particular
alternative to the standard model of cosmology shedding light into the nature
of the mysterious dark matter.
