The Globular Cluster Systems of Ultra-Diffuse Galaxies in the Coma Cluster

TL;DR

This study investigates the globular cluster systems of ultra-diffuse galaxies in the Coma cluster, revealing diverse properties and environmental dependencies that suggest multiple formation pathways.

Contribution

It provides a comprehensive analysis of GC populations in UDGs and dwarfs, highlighting differences in GC frequency and environment-related trends, which are novel insights into UDG formation.

Findings

Higher GC specific frequency in UDGs compared to dwarfs.

GC frequency correlates with galaxy size and environment.

Diversity in GC abundance suggests multiple formation mechanisms.

Abstract

Ultra-diffuse galaxies (UDGs) are unusual galaxies with low luminosities, similar to classical dwarf galaxies, but sizes up to $\sim\!5$ larger than expected for their mass. Some UDGs have large populations of globular clusters (GCs), something unexpected in galaxies with such low stellar density and mass. We have carried out a comprehensive study of GCs in both UDGs and classical dwarf galaxies at comparable stellar masses using HST observations of the Coma cluster. We present new imaging for 33 Dragonfly UDGs with the largest effective radii ($>2$ kpc), and additionally include 15 UDGs and 54 classical dwarf galaxies from the HST/ACS Coma Treasury Survey and the literature. Out of a total of 48 UDGs, 27 have statistically significant GC systems, and 11 have candidate nuclear star clusters. The GC specific frequency ($S_N$) varies dramatically, with the mean $S_N$ being higher for UDGs than for classical dwarfs. At constant stellar mass, galaxies with larger sizes (or lower surface brightnesses) have higher $S_N$, with the trend being stronger at higher stellar mass. At lower stellar masses, UDGs tend to have higher $S_N$ when closer to the center of the cluster, i.e., in denser environments. The fraction of UDGs with a nuclear star cluster also depends on environment, varying from $\sim\!40$\% in the cluster core, where it is slightly lower than the nucleation fraction of classical dwarfs, to $\lesssim20\%$ in the outskirts. Collectively, we observe an unmistakable diversity in the abundance of GCs, and this may point to multiple formation routes.