Superfluid Dark Matter around Black Holes

TL;DR

This paper investigates the density profile of superfluid dark matter around supermassive black holes, revealing distinct behaviors that could differentiate it from collisionless dark matter in galactic centers.

Contribution

It provides the first detailed computation of superfluid dark matter profiles near black holes, highlighting how different equations of state affect the density distribution.

Findings

Dark matter profile exhibits distinct power-law behaviors near black holes.

Profiles depend on the fluid's equation of state, enabling potential observational tests.

Superfluid dark matter can be distinguished from collisionless dark matter in galactic centers.

Abstract

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.