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 .