Rotating galactic black holes

TL;DR

This paper develops a new fully-relativistic formalism to model rotating galactic black holes within axisymmetric, non-vacuum spacetimes, aiding the understanding of their environment and observable phenomena.

Contribution

It introduces a novel formalism for solutions of Einstein's gravity coupled with anisotropic fluids in axisymmetric spacetimes, extending previous spherically symmetric models.

Findings

Formalism describes regular horizons in asymptotically flat spacetimes

Framework can model the geometry of galaxies with supermassive black holes

Provides groundwork for studying black hole shadows and quasi-normal modes

Abstract

The galactic black hole is a supermassive black hole located at the center of a galaxy surrounded by a dark matter halo. For the first time, we establish a generic, fully-relativistic formalism to calculate solutions of Einstein's gravity minimally coupled to an anisotropic fluid modeled by the Einstein cluster in axisymmetric, non-vacuum spacetimes, which are extensions of spherically-symmetric cases. These asymptotically flat spacetimes with regular horizons can describe the geometry of galaxies harboring supermassive black holes and are useful to constrain the environment surrounding astrophysical black holes. Our findings provide a solid groundwork for future studies on the shadows, quasi-normal modes, and other phenomena associated with rotating galactic black holes.