Howes, L.M.Asplund, M.Casey, A.R.Keller, S.C.Yong, D.Gilmore, G.Lind, K.Worley, C.Bessell, M.S.Casagrande, L.Marino, A.F.Nataf, D.M.Owen, C.I.Da Costa, G.S.Schmidt, B.P.Tisserand, P.Randich, S.Feltzing, S.Vallenari, A.Allende Prieto, C.Bensby, T.Flaccomio, E.Korn, A.J.Pancino, E.Recio-Blanco, A.Smiljanic, R.Bergemann, M.Costado, M.T.Damiani, F.Heiter, U.Hill, V.Hourihane, A.Jofré, P.Lardo, C.de Laverny, P.Magrini, L.Maiorca, E.Masseron, T.Morbidelli, L.Sacco, G.G.Minniti, D.Zoccali, M.2023-05-302023-05-302014-09Monthly Notices of the Royal Astronomical Society. sVolume 445, Issue 4, Pages 4241 - 4246. 29 September 20140035-8711https://repositorio.unab.cl/xmlui/handle/ria/50118Indexación: Scopus.We present the first results of the EMBLA survey (Extremely Metal-poor BuLge stars with AAOmega), aimed at finding metal-poor stars in the Milky Way bulge, where the oldest stars should now preferentially reside. EMBLA utilizes SkyMapper photometry to pre-select metal-poor candidates, which are subsequently confirmed using AAOmega spectroscopy. We describe the discovery and analysis of four bulge giants with −2.72 ≤ [Fe/H] ≤ −2.48, the lowest metallicity bulge stars studied with high-resolution spectroscopy to date. Using FLAMES/UVES spectra through the Gaia-ESO Survey we have derived abundances of twelve elements. Given the uncertainties, we find a chemical similarity between these bulge stars and halo stars of the same metallicity, although the abundance scatter may be larger, with some of the stars showing unusual [α/Fe] ratios.enStars: AbundancesStars: Population IIGalaxy: BulgeGalaxy: EvolutionArtículoAtribution 4.0 International (CC BY 4.0)DOI: 10.1093/mnras/stu1991