Title: The K2 Galactic Archaeology Program Data Release 3: Age-abundance Patterns in C1–C8 and C10–C18

Journal Article · · The Astrophysical Journal
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  1. American Museum of Natural History (AMNH), New York, NY (United States); Univ. of New South Wales, Sydney, NSW (Australia)
  2. Univ. of New South Wales, Sydney, NSW (Australia); Univ. of Sydney, NSW (Australia); Aarhus Univ. (Denmark); ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) (Australia)
  3. Aarhus Univ. (Denmark); Univ. of Birmingham (United Kingdom)
  4. Centre National de la Recherche Scientifique (CNRS) (France); Univ. Paris-Saclay, Gif-sur-Yvette (France); University Paris-Diderot (France); Sorbonne Univ., Paris (France)
  5. Univ. of Vienna (Austria)
  6. Instituto de Astrofísica de Canarias, La Laguna, Tenerife (Spain); Universidad de La Laguna, Tenerife (Spain)
  7. Paris Observatory, Paris (France). Laboratory for Space Science and Astrophysical Instrumentation (LESIA); PSL Research University, Paris (France); Sorbonne Univ., Paris (France); University Paris-Diderot (France); Centre National de la Recherche Scientifique (CNRS) (France)
  8. Univ. of New South Wales, Sydney, NSW (Australia)
  9. Centre National de la Recherche Scientifique (CNRS) (France); Univ. Paris-Saclay, Gif-sur-Yvette (France); University Paris-Diderot (France); Sorbonne Univ., Paris (France); Flatiron Institute, New York, NY (United States). Simons Foundation
  10. Univ. of Birmingham (United Kingdom)
  11. Univ. of Sydney, NSW (Australia); ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) (Australia)
  12. Univ. College London, Surrey (United Kingdom). Mullard Space Science Lab. (MSSL)
  13. The Ohio State Univ., Columbus, OH (United States)
  14. Flatiron Institute, New York, NY (United States); Univ. of Washington, Seattle, WA (United States)
  15. Univ. of Texas, Austin, TX (United States)
  16. University of Hertfordshire, Hatfield (United Kingdom)
  17. Univ. of Hawaii, Honolulu, HI (United States)
  18. ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) (Australia); Australian National Univ., Canberra, ACT (Australia)
  19. Univ. of Sydney, NSW (Australia); ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) (Australia); Australian National Univ., Canberra, ACT (Australia)
  20. Australian National Univ., Canberra, ACT (Australia). Mount Stromlo Observatory
  21. Univ. of Sydney, NSW (Australia)
  22. ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) (Australia); Australian National Univ., Canberra, ACT (Australia); Macquarie Univ., NSW (Australia)
  23. Aarhus Univ. (Denmark)
+ Show Author Affiliations

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, κR and κM, 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 κR and κM 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.

Research Organization:
US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)
Sponsoring Organization:
Danish National Research Foundation; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF); Science and Technology Facilities Council (STFC); Spanish Ministry of Science and Innovation (MCIN); USDOE Office of Science (SC)
OSTI ID:
1983199
Journal Information:
The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 2 Vol. 926; ISSN 0004-637X
Publisher:
IOP PublishingCopyright Statement
Country of Publication:
United States
Language:
English

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79 ASTRONOMY AND ASTROPHYSICS
Asteroseismology
Astronomy & Astrophysics
Galactic archaeology
Nucleosynthesis
R-process
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S-process
Stellar ages