Chemical evolution of the Galactic bulge as traced by microlensed dwarf and subgiant stars: VI. Age and abundance structure of the stellar populations in the central sub-kpc of the Milky Way

Research output: Contribution to journalArticle

Abstract

We present a detailed elemental abundance study of 90 F and G dwarf, turn-off, and subgiant stars in the Galactic bulge. Based on high-resolution spectra acquired during gravitational microlensing events, stellar ages and abundances for 11 elements (Na, Mg, Al, Si, Ca, Ti, Cr, Fe, Zn, Y and Ba) have been determined. Four main findings are presented: (1) a wide metallicity distribution with distinct peaks at [Fe/H] = -1.09, -0.63, -0.20, + 0.12, + 0.41; (2) a highfraction of intermediate-age to young stars where at [Fe/H] > 0 more than 35% are younger than 8 Gyr, and for [Fe/H] ≲-0.5 most stars are 10 Gyr or older; (3) several episodes of significant star formation in the bulge has been identified: 3, 6, 8, and 11 Gyr ago; (4) tentatively the "knee" in the α-element abundance trends of the sub-solar metallicity bulge is located at a slightly higher [Fe/H] than in the local thick disk. These findings show that the Galactic bulge has complex age and abundance properties that appear to be tightly connected to the main Galactic stellar populations. In particular, the peaks in the metallicity distribution, the star formation episodes, and the abundance trends, show similarities with the properties of the Galactic thin and thick disks. At the same time, the star formation rate appears to have been slightly faster in the bulge than in the local thick disk, which most likely is an indication of the denser stellar environment closer to the Galactic centre. There are also additional components not seen outside the bulge region, and that most likely can be associated with the Galactic bar. Our results strengthen the observational evidence that support the idea of a secular origin for the Galactic bulge, formed out of the other main Galactic stellar populations present in the central regions of our Galaxy. Additionally, our analysis of this enlarged sample suggests that the (V-I)0 colour of the bulge red clump should be revised to 1.09.

Details

Authors
  • A. Gould
  • J. C. Yee
  • J. A. Johnson
  • M. Asplund
  • J. Meléndez
  • S. Lucatello
  • A. McWilliam
  • A. Udalski
  • M. K. Szymański
  • I. Soszyński
  • R. Poleski
  • A. Wyrzykowski
  • K. Ulaczyk
  • S. Kozłowski
  • P. Pietrukowicz
  • J. Skowron
  • P. Mróz
  • J. M. Pawlak
  • F. Abe
  • Y. Asakura
  • A. Bhattacharya
  • I. A. Bond
  • D. P. Bennett
  • Y. Hirao
  • M. Nagakane
  • N. Koshimoto
  • T. Sumi
  • D. Suzuki
  • P. J. Tristram
Organisations
External organisations
  • Max Planck Institute for Astronomy
  • Ohio State University
  • Smithsonian Astrophysical Observatory
  • Australian National University
  • University of São Paulo
  • INAF - Osservatorio Astronomico di Padova
  • University of Warsaw
  • University of Warwick
  • Nagoya University
  • University of Notre Dame
  • Massey University
  • Osaka University
  • Mt. John University Observatory
  • Korea Astronomy and Space Science Institute (KASI)
  • Carnegie Observatories
  • NASA Goddard Space Flight Center
Research areas and keywords

Subject classification (UKÄ) – MANDATORY

  • Astronomy, Astrophysics and Cosmology

Keywords

  • Galaxy: bulge, Galaxy: evolution, Galaxy: formation, Gravitational lensing: micro, Stars: abundances
Original languageEnglish
Article numberA89
JournalAstronomy and Astrophysics
Volume605
Publication statusPublished - 2017 Sep 1
Publication categoryResearch
Peer-reviewedYes

Related activities

Feltzing, S. (First/primary/lead supervisor)
2015 Aug 12019 Feb 28

Activity: Examination and supervisionSupervision of PostDoc

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