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