Thanks to ongoing efforts to compute precise stellar ages, we can now characterize stars across different regions of the Milky Way. The Gaia and Kepler space missions, along with ground-based spectroscopic surveys like APOGEE, offer a unique opportunity to investigate chemo-kinematical relationships as a function of age within Galactic stellar populations, providing valuable insights for Galactic evolution models. In this poster, we discuss a sample of stars with measured chemical and seismic properties from the APOGEE spectroscopic survey and the Kepler satellite. Furthermore, astrometry data from the Gaia satellite is accessible for the majority of our sample. Given the model-dependent nature of ages inferred from asteroseismology, we compare results obtained from different age determinations from the APOKASC catalog (Pinsonneault et al., 2018) and Miglio et al. (2021). We explore the age-chemo-kinematic relationships within our sample's stellar populations using both sets of stellar ages, and compare them to simulations computed with the Besançon stellar population synthesis model. This comparison allows us to avoid the selection bias of the 2 sets. Among the various aspects covered, we discuss the characteristics of stars within the high-alpha metal-rich thick disc. Additionally, we examine the patterns in vertical velocity dispersion with stellar age for the high-alpha metal-poor thick disc, hinting at a more intricate chemo-dynamical scenario, likely influenced by mergers and radial migration effects.
N. Lagarde (Mon,) studied this question.