Alencastro Puls, ArthurCasagrande, LucaMonty, StephanieYong, DavidLiu, FanStello, DennisLund, Mikkel2025-01-092025-01-090035-8711https://hdl.handle.net/1885/733731550In this study we combine asteroseismic, spectroscopic, and kinematic information to perform a detailed analysis of a sample of 16 stars from the Kepler field. Our selection focuses on stars that appear to contradict Galactic chemical evolution models: young and α-rich, old and metal-rich, as well as other targets with unclear classification in past surveys. Kinematics are derived from Gaia DR3 parallaxes and proper motions, and high-resolution spectra from HIRES/Keck are used to calculate chemical abundances for over 20 elements. This information is used to perform careful checks on asteroseismic masses and ages derived via grid-based modelling. Among the seven stars previously classified as young and α-rich, only one seems to be an unambiguously older object masking its true age. We confirm the existence of two very old (≥11 Gyr), super metal-rich (≥0.1 dex) giants. These two stars have regular thin disc chemistry and in-plane solar circle orbits that fit well in the picture of radial migration via the churning mechanism. The alternative explanation that these stars have younger ages would require mass-loss rates that strongly increase with increasing metallicity. Finally, we suggest further investigations to explore the suitability of Zn as a chemical clock in red giants.Parts of this research were conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) through project number CE170100013. AAP acknowledges the support by the State of Hesse within the Research Cluster ELEMENTS (Project ID 500/10.006). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no. DNRF106).application/pdfen-AU© 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Societystars: fundamental parametersGalaxy: abundancesGalaxy: kinematics and dynamics202310.1093/mnras/stad13652024-01-14