2MASS J05575891-7258426 , the SIMBAD biblio

This paper presents the chemical abundance analysis of a sample of 27 red giant stars located in four populous intermediate-age globular clusters in the Large Magellanic Cloud, namely NGC 1651, 1783, 1978, and 2173. This analysis is based on high-resolution (R∼ 47,000) spectra obtained with the UVES@VLT spectrograph. For each cluster we derived up to 20 abundance ratios sampling the main chemical elemental groups, namely light odd-Z, α, iron-peak, and neutron-capture elements. All the analyzed abundance patterns behave similarly in the four clusters and also show negligible star-to-star scatter within each cluster. We find [Fe/H] = -0.30±0.03, -0.35±0.02, -0.38±0.02, and -0.51±0.03 dex for NGC 1651, 1783, 1978, and 2173, respectively. The measurement of light odd-Z nuclei gives slightly subsolar [Na/Fe] and a more significant [Al/Fe] depletion (~-0.50 dex). The [α/Fe] abundance ratios are nearly solar, while the iron-peak elements well trace those of the iron. S-process elements behave in a peculiar way: light s-elements give subsolar [Y/Fe] and [Zr/Fe] abundance ratios, while heavy s-elements give enhanced [Ba/Fe], [La/Fe], and [Nd/Fe] with respect to the solar values. Also, the [Eu/Fe] abundance ratio turns out to be enhanced (∼0.4 dex).