  In 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 $\alpha$-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 $\alpha$-rich, only one seems to be an
unambiguously older object masking its true age. We confirm the existence of
two very old ($\geq$11 Gyr), super metal rich ($\geq$0.1 dex) giants. These two
stars have regular thin disc chemistry and in-plane solar circle orbits which
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 which strongly increases with increasing metallicity. Finally,
we suggest further investigations to explore the suitability of Zn as a
chemical clock in red giants.
