Bensby, T.T.BensbyFeltzing, S.S.FeltzingGould, A.A.GouldYee, J. C.J. C.YeeJohnson, J. A.J. A.JohnsonAsplund, M.M.AsplundMeléndez, J.J.MeléndezLUCATELLO, SaraSaraLUCATELLOHowes, L. M.L. M.Howes2021-02-182021-02-182018978-1-107-19234-81743-9213http://hdl.handle.net/20.500.12386/30461The four main findings about the age and abundance structure of the Milky Way bulge based on microlensed dwarf and subgiant stars are: (1) a wide metallicity distribution with distinct peaks at [Fe/H] = -1.09, -0.63, -0.20, +0.12, +0.41; (2) a high fraction of intermediate-age to young stars where at [Fe/H] > 0 more than 35 % are younger than 8 Gyr, (3) several episodes of significant star formation in the bulge 3, 6, 8, and 11 Gyr ago; (4) the `knee' in the α-element abundance trends of the sub-solar metallicity bulge appears to be located at a slightly higher [Fe/H] (about 0.05 to 0.1 dex) than in the local thick disk.STAMPAenConference paper10.1017/S17439213170074262-s2.0-85060099154https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/age-and-abundance-structure-of-the-stellar-populations-in-the-central-subkpc-of-the-milky-way/CCBE7FE63592073DFB10E8B9028028D02018IAUS..334...86BFIS/05 - ASTRONOMIA E ASTROFISICA