  The idea of self-interacting bosonic dark matter capable of exhibiting
superfluidity is revisited. We show that the most interesting parameter space
of the theory corresponds to fully thermalized dark matter halos. As a result
the entire halo undergoes Bose-Einstein condensation due to high degeneracy.
Since it is observationally preferable for the dark matter density profile to
be similar to cold dark matter in the outskirts of the halo, we argue that the
Jeans wavelength must be at least few times shorter than the virial radius.
This entails that, upon condensation, a dark matter halo fragments into
superfluid clumps. However, we demonstrate that these would-be solitons
experience strong tidal disruption and behave as virialized weakly interacting
streams. An exception is the central soliton, which can be as large as few tens
of kiloparsecs in size without contradicting observational bounds. As a result,
in dwarf galaxies, the observed rotation curves can be completely contained
within the superfluid soliton. In this case, the dark matter distribution is
expected to be strongly sensitive to the baryonic density profile. We argue
that the diversity of rotation curves observed for dwarf galaxies is a natural
consequence of the superfluid dark matter scenario.
