  The tidal disruption of the Sagittarius dwarf Spheroidal galaxy (Sgr dSph) is
producing the most prominent substructure in the Milky Way (MW) halo, the
Sagittarius Stream. Aside from field stars, the Sgr dSph is suspected to have
lost a number of globular clusters (GC). Many Galactic GC are suspected to have
originated in the Sgr dSph. While for some candidates an origin in the Sgr dSph
has been confirmed due to chemical similarities, others exist whose chemical
composition has never been investigated. NGC 5053 and NGC 5634 are two among
these scarcely studied Sgr dSph candidate-member clusters. To characterize
their composition we analyzed one giant star in NGC 5053, and two in NGC 5634.
We analize high-resolution and signal-to-noise spectra by means of the MyGIsFOS
code, determining atmospheric parameters and abundances for up to 21 species
between O and Eu. The abundances are compared with those of MW halo field
stars, of "unassociated" MW halo globulars, and of the metal poor Sgr dSph main
body population.
  We derive a metallicity of [FeII/H]=-2.26+-0.10 for NGC 5053, and of
[FeI/H]=-1.99+-0.075 and -1.97+-0.076 for the two stars in NGC 5634. This makes
NGC 5053 one of the most metal poor globular clusters in the MW. Both clusters
display an alpha enhancement similar to the one of the halo at comparable
metallicity. The two stars in NGC 5634 clearly display the Na-O anticorrelation
widespread among MW globulars. Most other abundances are in good agreement with
standard MW halo trends. The chemistry of the Sgr dSph main body populations is
similar to the one of the halo at low metallicity. It is thus difficult to
discriminate between an origin of NGC 5053 and NGC 5634 in the Sgr dSph, and
one in the MW. However, the abundances of these clusters do appear closer to
that of Sgr dSph than of the halo, favoring an origin in the Sgr dSph system.
