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

Bensby, T. LU orcid ; Feltzing, S. LU orcid ; Gould, A. ; Yee, J. C. ; Johnson, J. A. ; Asplund, M. ; Meléndez, J. ; Lucatello, S. and Howes, L. M. LU (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:
author
; ; ; ; ; ; ; and
organization
publishing date
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
2022-10-16 03:30:49
@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] &gt; 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}},
}