  Cosmological models predict the oldest stars in the Galaxy should be found
closest to the centre of the potential well, in the bulge. The EMBLA Survey
successfully searched for these old, metal-poor stars by making use of the
distinctive SkyMapper photometric filters to discover candidate metal-poor
stars in the bulge. Their metal-poor nature was then confirmed using the
AAOmega spectrograph on the AAT. Here we present an abundance analysis of 10
bulge stars with -2.8<[Fe/H]<-1.7 from MIKE/Magellan observations, in total
determining the abundances of 22 elements. Combining these results with our
previous high-resolution data taken as part of the Gaia-ESO Survey, we have
started to put together a picture of the chemical and kinematic nature of the
most metal-poor stars in the bulge. The currently available kinematic data is
consistent with the stars belonging to the bulge, although more accurate
measurements are needed to constrain the stars' orbits. The chemistry of these
bulge stars deviates from that found in halo stars of the same metallicity. Two
notable differences are the absence of carbon-enhanced metal-poor bulge stars,
and the alpha-element abundances exhibit a large intrinsic scatter and include
stars which are underabundant in these typically enhanced elements.
