Gas-rich, field ultra-diffuse galaxies host few globular clusters

TL;DR

This study uses Hubble imaging to show that gas-rich, field ultra-diffuse galaxies host very few globular clusters, indicating different formation pathways from cluster UDGs and suggesting they are an extension of dwarf galaxies.

Contribution

It provides the first detailed analysis of globular cluster populations in gas-rich, field UDGs, revealing their scarcity of GCs and implications for UDG formation theories.

Findings

Field UDGs host very few globular clusters.

Most have zero candidate GCs, some have one or two.

Results suggest multiple formation pathways for UDGs.

Abstract

We present Hubble Space Telescope imaging of 14 gas-rich, low surface brightness galaxies in the field at distances of 25-36 Mpc, with mean effective radii and $g$-band central surface brightnesses of 1.9 kpc and 24.2 mag arcsec$^{-2}$. Nine meet the standard criteria to be considered ultra-diffuse galaxies (UDGs). An inspection of point-like sources brighter than the turnover magnitude of the globular cluster luminosity function and within twice the half-light radii of each galaxy reveals that, unlike those in denser environments, gas-rich, field UDGs host very few old globular clusters (GCs). Most of the targets (nine) have zero candidate GCs, with the remainder having one or two candidates each. These findings are broadly consistent with expectations for normal dwarf galaxies of similar stellar mass. This rules out gas-rich, field UDGs as potential progenitors of the GC-rich UDGs that are typically found in galaxy clusters. However, some in galaxy groups may be directly accreted from the field. In line with other recent results, this strongly suggests that there must be at least two distinct formation pathways for UDGs, and that this sub-population is simply an extreme low surface brightness extension of the underlying dwarf galaxy population. The root cause of their diffuse stellar distributions remains unclear, but the formation mechanism appears to only impact the distribution of stars (and potentially dark matter), without strongly impacting the distribution of neutral gas, the overall stellar mass, or the number of GCs.