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Similarities in the chemical composition of two of the closest Milky Waysatellites, namely the Large Magellanic Cloud (LMC) and the Sagittarius (Sgr)dwarf galaxy, have been proposed in the literature, suggesting similar chemicalenrichment histories between the two galaxies. This proposition, however, restson different abundance analyses, which likely introduce various systematicsthat hamper a fair comparison among the different data sets. In order to bypassthis issue (and highlight real similarities and differences between theirabundance patterns), we present a homogeneous chemical analysis of 30 giantstars in LMC, 14 giant stars in Sgr and 14 giants in the Milky Way, based onhigh-resolution spectra taken with the spectrograph UVES-FLAMES. The LMC andSgr stars, in the considered metallicity range ([Fe/H]>-1.1 dex), show verysimilar abundance ratios for almost all the elements, with differences only inthe heavy s-process elements Ba, La and Nd, suggesting a different contributionby asymptotic giant branch stars. On the other hand, the two galaxies havechemical patterns clearly different from those measured in the Galactic stars,especially for the elements produced by massive stars. This finding suggeststhe massive stars contributed less to the chemical enrichment of these galaxieswith respect to the Milky Way. The derived abundances support similar chemicalenrichment histories for the LMC and Sgr.

A homogeneous comparison between the chemical composition of the Large Magellanic Cloud and the Sagittarius dwarf galaxy