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arXiv · 1707.05960

The age and abundance structure of the stellar populations in the central sub-kpc of the Milky Way

T. Bensby·S. Feltzing·A. Gould·J. C. Yee·J. A. Johnson·M. Asplund·J. Meléndez·S. Lucatello·L. M. Howes
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Abstract

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.

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T. Bensby, S. Feltzing, A. Gould, J. C. Yee, J. A. Johnson, M. Asplund, J. Meléndez, S. Lucatello, L. M. Howes. 2017-07-19. The age and abundance structure of the stellar populations in the central sub-kpc of the Milky Way. https://doi.org/10.1017/s1743921317007426

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