The K2 Galactic Archaeology Program Data Release 3

Autor(en): Joel C. Zinn, Dennis Stello, Yvonne Elsworth, Rafael A. García, Thomas Kallinger, Savita Mathur, Benoit Mosser, Marc Hon, Lisa Bugnet, Caitlin Jones, Claudia Reyes, Sanjib Sharma, Ralph Schönrich, Jack T. Warfield, Rodrigo Luger, Andrew Vanderburg, Chiaki Kobayashi, Marc H. Pinsonneault, Jennifer A. Johnson, Daniel Huber, Sven Buder, Meridith Joyce, Joss Bland-Hawthorn, Luca Casagrande, Geraint F. Lewis, Andrea Miglio, Thomas Nordlander, Guy R. Davies, Gayandhi De Silva, William J. Chaplin, Victor Silva Aguirre
Abstrakt: We present the third and final data release of the K2 Galactic Archaeology Program (K2 GAP) for Campaigns C1-C8 and C10-C18. We provide asteroseismic radius and mass coefficients, κ_R and κ_M, for ~19,000 red giant stars, which translate directly to radius and mass given a temperature. As such, K2 GAP DR3 represents the largest asteroseismic sample in the literature to date. K2 GAP DR3 stellar parameters are calibrated to be on an absolute parallactic scale based on Gaia DR2, with red giant branch and red clump evolutionary state classifications provided via a machine-learning approach. Combining these stellar parameters with GALAH DR3 spectroscopy, we determine asteroseismic ages with precisions of ~20%-30% and compare age-abundance relations to Galactic chemical evolution models among both low- and high-α populations for α, light, iron-peak, and neutron-capture elements. We confirm recent indications in the literature of both increased Ba production at late Galactic times as well as significant contributions to r-process enrichment from prompt sources associated with, e.g., core-collapse supernovae. With an eye toward other Galactic archeology applications, we characterize K2 GAP DR3 uncertainties and completeness using injection tests, suggesting that K2 GAP DR3 is largely unbiased in mass/age, with uncertainties of 2.9% (stat.) ± 0.1% (syst.) and 6.7% (stat.) ± 0.3% (syst.) in κ _R and κ _M for red giant branch stars and 4.7% (stat.) ± 0.3% (syst.) and 11% (stat.) ± 0.9% (syst.) for red clump stars. We also identify percent-level asteroseismic systematics, which are likely related to the time baseline of the underlying data, and which therefore should be considered in TESS asteroseismic analysis.
Organisation(en): Institut für Astrophysik
Externe Organisation(en): American Museum of Natural History, University of New South Wales, The University of Sydney, Aarhus University, ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), University of Birmingham, Université Paris Saclay, Instituto de Astrofísica de Canarias (IAC), Universidad de La Laguna, Université de recherche Paris Sciences et Lettres, Flatiron Institute, University College London, Ohio State University, University of Washington, University of Texas, Austin, University of Hertfordshire, University of Hawaii, Australian National University, Macquarie University
Journal: The Astrophysical Journal
Band: 926
Anzahl der Seiten: 34
ISSN: 0004-637X
DOI: https://doi.org/10.3847/1538-4357/ac2c83
Publikationsdatum: 02-2022
Peer-reviewed: Ja
ÖFOS 2012: 103003 Astronomie, 103004 Astrophysik
Schlagwörter
ASJC Scopus Sachgebiete: Astronomy and Astrophysics, Space and Planetary Science
Link zum Portal: https://ucrisportal.univie.ac.at/de/publications/31913722-1e08-424a-90dc-8f6147881121

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