The browser you are using is not supported by this website. All versions of Internet Explorer are no longer supported, either by us or Microsoft (read more here: https://www.microsoft.com/en-us/microsoft-365/windows/end-of-ie-support).

Please use a modern browser to fully experience our website, such as the newest versions of Edge, Chrome, Firefox or Safari etc.

Profile picture Diane Feuillet

Diane Feuillet

Researcher

Profile picture Diane Feuillet

Exploring the stellar age distribution of the milky way bulge using APOGEE

Author

  • Sten Hasselquist
  • Gail Zasowski
  • Diane K. Feuillet
  • Mathias Schultheis
  • David M. Nataf
  • Borja Anguiano
  • Rachael L. Beaton
  • Timothy C. Beers
  • Roger E. Cohen
  • Katia Cunha
  • José G. Fernández-Trincado
  • D. A. García-Hernández
  • Doug Geisler
  • Jon A. Holtzman
  • Jennifer Johnson
  • Richard R. Lane
  • Steven R. Majewski
  • Christian Moni Bidin
  • Christian Nitschelm
  • Alexandre Roman-Lopes
  • Ricardo Schiavon
  • Verne V. Smith
  • Jennifer Sobeck
Show all

Summary, in English

We present stellar age distributions of the Milky Way bulge region using ages for ∼6000 high-luminosity (log(g)< 2.0), metal-rich ([Fe/H] ≥ -0.5) bulge stars observed by the Apache Point Observatory Galactic Evolution Experiment. Ages are derived using The Cannon label-transfer method, trained on a sample of nearby luminous giants with precise parallaxes for which we obtain ages using a Bayesian isochrone-matching technique. We find that the metal-rich bulge is predominantly composed of old stars (>8 Gyr). We find evidence that the planar region of the bulge (ZGC| 0.25 kpc) is enriched in metallicity, Z, at a faster rate (dZ/dt ∼ 0.0034 Gyr-1) than regions farther from the plane (dZ/dt ∼ 0.0013 Gyr-1 at | ZGC| > 1.00 kpc). We identify a nonnegligible fraction of younger stars (age ∼2-5 Gyr) at metallicities of +0.2 < [Fe/H] < +0.4. These stars are preferentially found in the plane (ZGC| ≤ 0.25 kpc) and at R cy ≈ 2-3 kpc, with kinematics that are more consistent with rotation than are the kinematics of older stars at the same metallicities. We do not measure a significant age difference between stars found inside and outside the bar. These findings show that the bulge experienced an initial starburst that was more intense close to the plane than far from the plane. Then, star formation continued at supersolar metallicities in a thin disk at 2 kpc ≲ R cy ≲ 3 kpc until ∼2 Gyr ago.

Department/s

  • Lund Observatory - Has been reorganised
  • eSSENCE: The e-Science Collaboration

Publishing year

2020

Language

English

Publication/Series

Astrophysical Journal

Volume

901

Issue

2

Document type

Journal article

Publisher

American Astronomical Society

Topic

  • Astronomy, Astrophysics and Cosmology

Status

Published

ISBN/ISSN/Other

  • ISSN: 0004-637X