  We present the dynamics of rotating Bose Condensate galactic dark matter
halos, made of an ultralight spinless boson. We restrict to the case of adding
axisymmetric rigid rotation to initially spherically symmetric structures and
show there are three regimes: i) small angular momentum, that basically retains
the drawbacks of spherically symmetric halos related to compactness and failure
at explaining galactic RCs, ii) an intermediate range of values of angular
momentum that allow the existence of long-lived structures with acceptable RC
profiles, and iii) high angular momentum, in which the structure is dispersed
away by rotation. We also present in detail the new code used to solve the
Gross-Pitaevskii Poisson system of equations in three dimensions.
