# Stellar-Mass Black Holes in Globular Clusters: Dynamical Consequences and Observational Signatures

## TL;DR

This paper investigates how stellar-mass black holes influence globular cluster evolution and observational features, using numerical simulations to identify key factors for BH retention and signatures of BH-rich clusters.

## Contribution

It identifies the main parameters affecting long-term black hole retention in globular clusters and proposes methods to observationally detect BH-rich clusters.

## Key findings

- BH retention depends on initial natal kicks and cluster properties
- BH-rich clusters tend to have low central brightness and large radii
- Methods are proposed to identify clusters with many black holes

## Abstract

Sizeable number of stellar-mass black holes (BHs) in globular clusters (GCs) can strongly influence the dynamical evolution and observational properties of their host cluster. Using results from a large set of numerical simulations, we identify the key ingredients needed to sustain a sizeable population of BHs in GCs up to a Hubble time. We find that while BH natal kick prescriptions are essential in determining the initial retention fraction of BHs in GCs, the long-term survival of BHs is determined by the size, initial central density and half-mass relaxation time of the GC. Simulated GC models that contain many BHs are characterized by relatively low central surface brightness, large half-light and core radii values. We also discuss novel ways to compare simulated results with available observational data to identify GCs that are most likely to contain many BHs.