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Cosmological models predict the oldest stars in the Galaxy should be foundclosest to the centre of the potential well, in the bulge. The EMBLA Surveysuccessfully searched for these old, metal-poor stars by making use of thedistinctive SkyMapper photometric filters to discover candidate metal-poorstars in the bulge. Their metal-poor nature was then confirmed using theAAOmega spectrograph on the AAT. Here we present an abundance analysis of 10bulge stars with -2.8<[Fe/H]<-1.7 from MIKE/Magellan observations, in totaldetermining the abundances of 22 elements. Combining these results with ourprevious high-resolution data taken as part of the Gaia-ESO Survey, we havestarted to put together a picture of the chemical and kinematic nature of themost metal-poor stars in the bulge. The currently available kinematic data isconsistent with the stars belonging to the bulge, although more accuratemeasurements are needed to constrain the stars' orbits. The chemistry of thesebulge stars deviates from that found in halo stars of the same metallicity. Twonotable differences are the absence of carbon-enhanced metal-poor bulge stars,and the alpha-element abundances exhibit a large intrinsic scatter and includestars which are underabundant in these typically enhanced elements.

The EMBLA Survey -- Metal-poor stars in the Galactic bulge