The age and abundance structure of the stellar populations in the central sub-kpc of the Milky Way
(2017) In Proceedings of the International Astronomical Union 13(S334). p.86-89- 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 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.
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/bdd1106e-33f8-4c77-8803-ad3b94127b2e
- author
- Bensby, T. LU ; Feltzing, S. LU ; Gould, A. ; Yee, J. C. ; Johnson, J. A. ; Asplund, M. ; Meléndez, J. ; Lucatello, S. and Howes, L. M. LU
- organization
- publishing date
- 2017
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- Galaxy: abundances, Galaxy: disk, Galaxy: evolution, Galaxy: structure
- in
- Proceedings of the International Astronomical Union
- volume
- 13
- issue
- S334
- pages
- 4 pages
- publisher
- Cambridge University Press
- external identifiers
-
- scopus:85060099154
- ISSN
- 1743-9213
- DOI
- 10.1017/S1743921317007426
- language
- English
- LU publication?
- yes
- id
- bdd1106e-33f8-4c77-8803-ad3b94127b2e
- alternative location
- https://arxiv.org/pdf/1707.05960.pdf
- date added to LUP
- 2019-02-12 11:06:21
- date last changed
- 2024-03-02 20:08:21
@article{bdd1106e-33f8-4c77-8803-ad3b94127b2e, abstract = {{<p>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 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.</p>}}, author = {{Bensby, T. and Feltzing, S. and Gould, A. and Yee, J. C. and Johnson, J. A. and Asplund, M. and Meléndez, J. and Lucatello, S. and Howes, L. M.}}, issn = {{1743-9213}}, keywords = {{Galaxy: abundances; Galaxy: disk; Galaxy: evolution; Galaxy: structure}}, language = {{eng}}, number = {{S334}}, pages = {{86--89}}, publisher = {{Cambridge University Press}}, series = {{Proceedings of the International Astronomical Union}}, title = {{The age and abundance structure of the stellar populations in the central sub-kpc of the Milky Way}}, url = {{http://dx.doi.org/10.1017/S1743921317007426}}, doi = {{10.1017/S1743921317007426}}, volume = {{13}}, year = {{2017}}, }