Toward the general RGB slope-metallicity-age calibration: I Metallicities, Ages and Kinematics for Eight LMC Clusters

TL;DR

This study provides spectroscopic metallicities, ages, and kinematic data for eight LMC clusters, revealing insights into their formation history, metallicity distribution, and rotational properties, with implications for understanding the LMC's evolution.

Contribution

First spectroscopic metallicity measurements for four LMC clusters, combined with age and kinematic analysis, offering new insights into cluster formation and LMC evolution.

Findings

Six clusters are 0.8-2.2 Gyr old with a tight metallicity distribution around -0.49.

The LMC exhibits disk-like rotation with no metallicity gradient.

No evidence of halo kinematics or metallicity gradient in the LMC.

Abstract

In this paper, we discuss the properties of CMDs, age, metallicity and radial velocities of eight massive LMC clusters using data taken from FORS2 multiobject spectrograph at the 8.2-meter VLT/UT1. The strong near-infrared Ca II triplet (CaT) lines of RGB stars obtained from the high S/N spectra are used to determine the metallicity and radial velocity of cluster members. We report for the first time spectroscopically determined metallicity values for four clusters based on the mean [Fe/H] value of ~10 cluster members each. We found two concentrations in the distribution of ages of the target clusters. Six have ages between 0.8-2.2 Gyr and the other two, NGC 1754 and NGC 1786, are very old. The metallicity of the six intermediate age clusters, with a mean age of 1.5 Gyr, is -0.49 with a scatter of only 0.04. This tight distribution suggests that a close encounter between the LMC and SMC may have caused not only the restart of cluster formation in the LMC but the generation of the central bar. The metallicity for the two old clusters is similar to that of the other old, metal-poor LMC clusters. We find that the LMC cluster system exhibits disk-like rotation with no clusters appearing to have halo kinematics and there is no evidence of a metallicity gradient in the LMC, in contrast with the stellar population of the MW and M33, where the metallicity decreases as galactocentric distance increases. The LMC's stellar bar may be the factor responsible for the dilution of any kind of gradient in the LMC.