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

doi:10.1017/S1743921317007426

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 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.

Original language	English
Pages (from-to)	86-89
Number of pages	4
Journal	Proceedings of the International Astronomical Union
Volume	13
Issue number	S334
DOIs	https://doi.org/10.1017/S1743921317007426
Publication status	Published - 2017

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

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.",

keywords = "Galaxy: abundances, Galaxy: disk, Galaxy: evolution, Galaxy: structure",

author = "T. Bensby and S. Feltzing and A. Gould and Yee, \{J. C.\} and Johnson, \{J. A.\} and M. Asplund and J. Mel{\'e}ndez and S. Lucatello and Howes, \{L. M.\}",

note = "Publisher Copyright: {\textcopyright} International Astronomical Union 2018.",

year = "2017",

doi = "10.1017/S1743921317007426",

language = "English",

volume = "13",

pages = "86--89",

journal = "Proceedings of the International Astronomical Union",

issn = "1743-9213",

publisher = "Cambridge University Press",

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TY - JOUR

T1 - The age and abundance structure of the stellar populations in the central sub-kpc of the Milky Way

AU - Bensby, T.

AU - Feltzing, S.

AU - Gould, A.

AU - Yee, J. C.

AU - Johnson, J. A.

AU - Asplund, M.

AU - Meléndez, J.

AU - Lucatello, S.

AU - Howes, L. M.

N1 - Publisher Copyright: © International Astronomical Union 2018.

PY - 2017

Y1 - 2017

N2 - 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.

AB - 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.

KW - Galaxy: abundances

KW - Galaxy: disk

KW - Galaxy: evolution

KW - Galaxy: structure

UR - https://www.scopus.com/pages/publications/85060099154

U2 - 10.1017/S1743921317007426

DO - 10.1017/S1743921317007426

M3 - Article

SN - 1743-9213

VL - 13

SP - 86

EP - 89

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

IS - S334

ER -

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

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