Mapping the Galactic centre's dark cluster via resonant relaxation

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. 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 supermassive black hole formation scenarios.

Automated summary

Supermassive black holes at the center of galaxies play a significant role in shaping the orbits of surrounding stellar clusters. Stars in these dense environments experience relaxation of their eccentricities through resonant and non-resonant processes, which can be explored using resonant diffusion coefficients. By studying the S-cluster around SgrA* and employing this framework, researchers can estimate the properties of intermediate-mass black holes and dark clusters, contributing to the understanding of supermassive black hole formation scenarios.