Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 475, Issue 4, Pages 5487-5500Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty150
Keywords
asteroseismology; stars: fundamental parameters; stars: kinematics and dynamic; Galaxy: disc; Galaxy: evolution; Galaxy: structure
Categories
Funding
- NASA's Science Mission Directorate
- Danish National Research Foundation [DNRF106]
- VILLUM FONDEN [10118]
- Australian Research Council Future Fellowship [FT160100402, FT1400147]
- UK's Science and Technology Facilities Council (STFC) [ST/N000811/1, ST/N504488/1]
- Danish Council for Independent Research - Natural Science [DFF-4181-00415]
- Australian Research Council [DE140101364]
- National Aeronautics and Space Administration [NNX14AB92G]
- NSF [AST-1211673]
- MINECO [ESP2015-66134-R]
- European Research Council under the European Union's Seventh Framework Programme (FP 7) ERC Grant [321035]
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- Center for High-Performance Computing at the University of Utah
- Carnegie Institution for Science
- Carnegie Mellon University
- Chilean Participation Group
- French Participation Group
- Harvard-Smithsonian Center for Astrophysics
- Instituto de Astrofisica de Canarias
- Johns Hopkins University
- Kavli Institute for the Physics and Mathematics of the Universe/University of Tokyo
- Lawrence Berkeley National Laboratory
- Leibniz Institut fur Astrophysik Potsdam
- Max-Planck-Institut fur Astronomie (Heidelberg)
- Max-Planck-Institut fur Astrophysik (Garching)
- Max-Planck-Institut fur Extraterrestrische Physik
- National Astronomical Observatories of China
- New Mexico State University
- New York University
- University of Notre Dame
- Observatrio Nacional/MCTI
- Ohio State University
- Pennsylvania State University
- Shanghai Astronomical Observatory
- United Kingdom Participation Group
- Universidad Nacional Autnoma de Mexico
- University of Arizona
- University of Colorado Boulder
- University of Oxford
- University of Portsmouth
- University of Utah
- University of Virginia
- University of Washington
- University of Wisconsin
- Vanderbilt University
- Yale University
- Astrophysical Research Consortium
- Science and Technology Facilities Council [ST/N000811/1] Funding Source: researchfish
- STFC [ST/N000811/1] Funding Source: UKRI
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Investigations of the origin and evolution of the Milky Way disc have long relied on chemical and kinematic identifications of its components to reconstruct our Galactic past. Difficulties in determining precise stellar ages have restricted most studies to small samples, normally confined to the solar neighbourhood. Here, we break this impasse with the help of asteroseismic inference and perform a chronology of the evolution of the disc throughout the age of the Galaxy. We chemically dissect the Milky Way disc population using a sample of red giant stars spanning out to 2 kpc in the solar annulus observed by the Kepler satellite, with the added dimension of asteroseismic ages. Our results reveal a clear difference in age between the low- and high-alpha populations, which also show distinct velocity dispersions in the V and W components. We find no tight correlation between age and metallicity nor [alpha/Fe] for the high-alpha disc stars. Our results indicate that this component formed over a period of more than 2 Gyr with a wide range of [M/H] and [alpha/Fe] independent of time. Our findings show that the kinematic properties of young a-rich stars are consistent with the rest of the high-alpha population and different from the low-alpha stars of similar age, rendering support to their origin being old stars that went through a mass transfer or stellar merger event, making them appear younger, instead of migration of truly young stars formed close to the Galactic bar.
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