http://arxiv.org/abs/1707.05960
The 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 alpha-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.
T. Bensby, S. Feltzing, A. Gould, et. al.
Thu, 20 Jul 17
51/56
Comments: 4 pages, contributed talk at the IAU Symposium 334 “Rediscovering our Galaxy” in Potsdam, July 10-14, 2017