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The tidal disruption of the Sagittarius dwarf Spheroidal galaxy (Sgr dSph) isproducing the most prominent substructure in the Milky Way (MW) halo, theSagittarius Stream. Aside from field stars, the Sgr dSph is suspected to havelost a number of globular clusters (GC). Many Galactic GC are suspected to haveoriginated in the Sgr dSph. While for some candidates an origin in the Sgr dSphhas been confirmed due to chemical similarities, others exist whose chemicalcomposition has never been investigated. NGC 5053 and NGC 5634 are two amongthese scarcely studied Sgr dSph candidate-member clusters. To characterizetheir 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 MyGIsFOScode, determining atmospheric parameters and abundances for up to 21 speciesbetween O and Eu. The abundances are compared with those of MW halo fieldstars, of "unassociated" MW halo globulars, and of the metal poor Sgr dSph mainbody 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 makesNGC 5053 one of the most metal poor globular clusters in the MW. Both clustersdisplay an alpha enhancement similar to the one of the halo at comparablemetallicity. The two stars in NGC 5634 clearly display the Na-O anticorrelationwidespread among MW globulars. Most other abundances are in good agreement withstandard MW halo trends. The chemistry of the Sgr dSph main body populations issimilar to the one of the halo at low metallicity. It is thus difficult todiscriminate between an origin of NGC 5053 and NGC 5634 in the Sgr dSph, andone in the MW. However, the abundances of these clusters do appear closer tothat of Sgr dSph than of the halo, favoring an origin in the Sgr dSph system.

Chemical abundances of giant stars in NGC 5053 and NGC 5634, two globular clusters associated with the Sagittarius dwarf Spheroidal galaxy?