Thanks to the ongoing efforts to compute accurate stellar ages, we are able to characterise stars in different regions of the Milky Way. The Gaia and Kepler space-missions, along with ground-based spectroscopic surveys such as APOGEE, provide a unique way to study the chemo-kinematical relations as function of age through the Galactic stellar populations, and provide new constraints to Galactic evolution model. In this poster, I present some results from Lagarde et al. (2021) where we study stars with measured chemical and seismic properties from APOGEE spectroscopic survey and the Kepler satellite, respectively. In addition, astrometry from the Gaia satellite is available for the majority of the sample. Because of the model-dependent nature of the 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). In this poster, I present the age-chemo-kinematical relations of the stellar populations observed in our sample using the both stellar ages ; and then compared to the simulations from the Besançon stellar populations synthesis model. Although the age distribution of the metal-rich high-α thick disc is similar to the metal-poor high-α thick disc, it seems to follow the kinematics of the thin disc. This feature suggests a different origin and history of these stars. Finally, we underline the inversion of the dispersion of the vertical velocity with age for the metal-poor high α thick disc, suggesting a more complex chemo-dynamical scheme, most likely including mergers and radial migration effects.< Réduire