Mapping the Galactic centre's dark cluster via Resonant Relaxation

TL;DR

This paper develops a resonant relaxation framework to map the dark stellar cluster around the Galactic centre's supermassive black hole, aiding in understanding the cluster's properties and black hole formation.

Contribution

It introduces an efficient method to explore stellar cluster parameters using resonant relaxation, constrained by recent S-cluster observations.

Findings

Estimated mass and cusp exponent of intermediate-mass black holes.

Constraints on the distribution of the unresolved stellar background.

Implications for supermassive black hole formation scenarios.

Abstract

Supermassive black holes in the centre of galaxies dominate the gravitational potential of their surrounding stellar clusters. In these dense environments, stars follow nearly Keplerian orbits, which get slowly distorted as a result of the potential fluctuations generated by the stellar cluster itself as a whole. In particular, stars undergo a rapid relaxation of their eccentricities through both resonant and non-resonant processes. An efficient implementation of the resonant diffusion coefficients allows for detailed and systematic explorations of the parameter space describing the properties of the stellar cluster. In conjunction with recent observations of the S-cluster orbiting SgrA*, this framework can be used to jointly constrain the distribution of the unresolved, old, background stellar cluster and the characteristics of a putative dark cluster. Specifically, we show how this can be used to estimate the typical mass and cuspide exponent of intermediate-mass black holes consistent with the relaxed state of the distribution of eccentricities in the observed S-cluster. This should prove useful in constraining super massive black hole formation scenarios.