Detailed Chemical Abundances of Star Clusters in the Large Magellanic
  Cloud
  We derive the first detailed chemical abundances of three star clusters in
the Large Magellanic Cloud (LMC), NGC1831 (436+/-22 Myr), NGC1856 (350+/-18
Myr) and [SL63]268 (1230+/-62 Myr) using integrated-light spectroscopic
observations obtained with the Magellan Echelle spectrograph on Magellan Baade
telescope. We derive [Fe/H], [Mg/Fe], [Ti/Fe], [Ca/Fe], [Ni/Fe], [Mn/Fe],
[Cr/Fe] and [Na/Fe] for the three clusters. Overall, our results match the LMC
abundances obtained in the literature as well as those predicted by detailed
chemical evolution models. For clusters NGC1831 and NGC1856, the [Mg/Fe] ratios
appear to be slightly depleted compared to [Ca/Fe] and [Ti/Fe]. This could be
hinting at the well-known Mg-Al abundance anti-correlation observed in several
Milky Way globular clusters. We note, however, that higher signal-to-noise
observations are needed to confirm such a scenario, particularly for NGC 1831.
We also find a slightly enhanced integrated-light [Na/Fe] ratio for cluster
[SL63]268 compared to those from the LMC field stars, possibly supporting a
scenario of intracluster abundance variations. We stress that detailed
abundance analysis of individual stars in these LMC clusters is required to
confirm the presence or absence of MSPs.
