Stellar clusters associated with GAMA 526784. Left: HST RGB image with the identified clusters marked and numbered in white. Old clusters are shown as circles, while young ones are diamonds. Candidates have open markers and confirmed clusters have closed ones. The inset histogram on the left compares two theoretical luminosity functions: The red curve is the typical GCLF for old globular clusters, peaking at M_F814W = −8.2 mag, while the blue curve represents the luminosity function corrected for the younger clusters’ ages, with a peak at M_F814W = −9.9 mag. The grey histogram shows the magnitude distribution of the young stellar clusters, while the red one shows the old clusters. Right: BAGPIPES fits for a representative star-forming cluster (number 19) and an old globular cluster (number 10). The star cluster has a young age of t_M ∼ 10 Myr, and a relatively high stellar mass of log(M_⊙/M_⋆) ∼ 5.5. The globular cluster, alternatively, has an old age of t_M ∼ 8.8 Gyr, and a slightly higher stellar mass of log(M_⊙/M_⋆) ∼ 5.6.