GAMA 526784: the progenitor of a globular cluster-rich ultra-diffuse galaxy? I. Star clusters, stellar body and ionised gas properties

TL;DR

This study of the isolated ultra-diffuse galaxy GAMA526784 reveals its complex stellar populations, star cluster formation, and kinematic properties, suggesting recent interactions triggered localized star formation and the creation of young star clusters.

Contribution

It provides detailed analysis of GAMA526784's stellar populations, star clusters, and kinematics, linking recent interactions to star formation in an ultra-diffuse galaxy.

Findings

Old stellar core (~9.9 Gyr) with low metallicity ([M/H] ~ -1.0 dex)

Younger outskirts (~0.9 Gyr) with slightly lower metallicity ([M/H] ~ -1.2 dex)

Presence of young star clusters (8-11 Myr) and old globular clusters (~9 Gyr)

Abstract

Context. Ultra-diffuse galaxies (UDGs) are an intriguing population of galaxies. Despite their dwarf-like stellar masses and low surface brightness, they have large half-light radii and exhibit a diverse range of globular cluster (GC) populations. Some UDGs host many GCs while others have none, raising questions about the conditions under which star clusters (SC) form in dwarfs. GAMA526784, an isolated UDG with both an old stellar body and an extended star-forming (SF) front, including many young SCs, provides an exceptional case to explore the link between UDG evolution and star cluster formation. Aims. This study investigates the stellar populations, SCs, ionised gas, and kinematics of GAMA526784, focusing on its potential to form massive GCs and its connection to broader UDG formation scenarios. Methods. Imaging from HST and Subaru/HSC, alongside MUSE spectroscopy, were used to analyse the galaxy's morphology, chemical composition, and kinematics. A combination of SED fitting and full spectral fitting was applied. Results. GAMA526784's central stellar body exhibits a low-metallicity ([M/H] ~ -1.0 dex) and an old age (~9.9 Gyr). The outskirts are much younger (~0.9 Gyr), but slightly more metal-poor ([M/H] ~ -1.2 dex). The stellar kinematics show low velocity dispersions (~10 km/s) and a coherent rotational field, while the ionised gas exhibits higher dispersions (~50 km/s), a misaligned rotation axis (~20 deg) and localised SF, what could be suggestive of a recent interaction. The young SCs span ages of 8-11 Myr and masses of log(M*/Mo)~5.0, while the old GCs have ~9 Gyr and stellar masses of log(M*/Mo)~5.5. Conclusions. GAMA526784's properties point to interactions that triggered localised SF, leading to the formation of young SCs. Future observations of its molecular and neutral gas will help assess its environment, and the trigger of this SF episode.