Photometry of Magellanic Cloud clusters with the Advanced Camera for Surveys - I. The old LMC clusters NGC 1928, 1939 and Reticulum

We present the results of photometric measurements from images of the LMC globular clusters NGC 1928, 1939 and Reticulum taken with the Advanced Camera for Surveys on the Hubble Space Telescope. Exposures through the F555W and F814W filters result in high accuracy colour-magnitude diagrams (CMDs) for these three clusters. This is the first time that CMDs for NGC 1928 and 1939 have been published. All three clusters possess CMDs with features indicating them to be > 10 Gyr old, including main sequence turn-offs at V ∼ 23 and well populated horizontal branches (HBs). We use the CMDs to obtain metallicity and reddening estimates for each cluster. NGC 1939 is a metal-poor cluster, with [Fe/H] = −2.10±0.19, while NGC 1928 is significantly more metal-rich, with [Fe/H] = −1.27 ± 0.14. The abundance of Reticulum is intermediate between the two, with [Fe/H] = −1.66 ± 0.12 – a measurement which matches well with previous estimates. All three clusters are moderately reddened, with values ranging from E(V − I) = 0.07 ± 0.02 for Reticulum and E(V − I) = 0.08 ± 0.02 for NGC 1928, to E(V − I) = 0.16 ± 0.03 for NGC 1939. After correcting the CMDs for extinction we estimate the HB morphology of each cluster. NGC 1928 and 1939 possess HBs consisting almost exclusively of stars to the blue of the instability strip, with NGC 1928 in addition showing evidence for an extended blue HB. In contrast, Reticulum has an intermediate HB morphology, with stars across the instability strip. Using a variety of dating techniques we show that these three clusters are coeval with each other and the oldest Galactic and LMC globular clusters, to within ∼ 2 Gyr. The census of known old LMC globular clusters therefore now numbers 15 plus the unique, somewhat younger cluster ESO121-SC03. The NGC 1939 field contains another cluster in the line-of-sight, NGC 1938. A CMD for this object shows it to be less than ∼ 400 Myr old, and it is therefore unlikely to be physically associated with NGC 1939.