  Superfluid dark matter, consisting of self-interacting light particles that
thermalize and condense to form a superfluid in galaxies, provides a novel
theory that matches the success of the standard $\Lambda$CDM model on
cosmological scales while simultaneously offering a rich phenomenology on
galactic scales. Within galaxies, the dark matter density profile consists of a
nearly homogeneous superfluid core surrounded by an isothermal envelope. In
this work we compute the density profile of superfluid dark matter around
supermassive black holes at the center of galaxies. We show that, depending on
the fluid equation of state, the dark matter profile presents distinct
power-law behaviors, which can be used to distinguish it from the standard
results for collisionless dark matter.
