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    Exploring the Stellar Age Distribution of the Milky Way Bulge Using APOGEE

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    Hasselquist_2020_ApJ_901_109.pdf
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    Author
    Hasselquist, Sten
    Zasowski, Gail
    Feuillet, Diane K.
    Schultheis, Mathias
    Nataf, David M.
    Anguiano, Borja
    Beaton, Rachael L.
    Beers, Timothy C.
    Cohen, Roger E.
    Cunha, Katia
    Fernández-Trincado, José G.
    García-Hernández, D. A.
    Geisler, Doug
    Holtzman, Jon A.
    Johnson, Jennifer
    Lane, Richard R.
    Majewski, Steven R.
    Bidin, Christian Moni
    Nitschelm, Christian
    Roman-Lopes, Alexandre
    Schiavon, Ricardo
    Smith, Verne V.
    Sobeck, Jennifer
    Show allShow less
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2020-09-28
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Hasselquist, S., Zasowski, G., Feuillet, D. K., Schultheis, M., Nataf, D. M., Anguiano, B., ... & Sobeck, J. (2020). Exploring the stellar age distribution of the Milky Way Bulge using APOGEE. The Astrophysical Journal, 901(2), 109.
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    © 2020. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    We present stellar age distributions of the Milky Way bulge region using ages for similar to 6000 high-luminosity (log (g), 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 (vertical bar Z(GC)vertical bar <= 0.25 kpc) is enriched in metallicity, Z, at a faster rate (dZ/dt similar to 0.0034 Gyr(-1)) than regions farther from the plane (dZ/dt similar to 0.0013 Gyr(-1) at vertical bar Z(GC)vertical bar > 1.00 kpc). We identify a nonnegligible fraction of younger stars (age similar to 2-5 Gyr) at metallicities of +0.2 < [Fe/H] < +0.4. These stars are preferentially found in the plane (vertical bar Z(GC)vertical bar <= 0.25 kpc) and at R-cy approximate to 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 less than or similar to R-cy less than or similar to 3 kpc until similar to 2 Gyr ago.
    ISSN
    0004-637X
    EISSN
    1538-4357
    DOI
    10.3847/1538-4357/abaeee
    Version
    Final published version
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/abaeee
    Scopus Count
    Collections
    UA Faculty Publications

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