In the era of large spectroscopic surveys, high-quality spectra can contribute to understand how our Galaxy formed and evolved until the present-day structure, not only providing high-precision abundances of elements belonging to the different nucleosynthesis channels, but also constraining one of the most elusive quantities in astrophysics, i.e., stellar age. Some abundance ratios, called chemical clocks, have proved to be excellent indicators of the stellar age. We can classify them into two families: ratios composed by elements whose surface abundances vary during stellar evolution, such as [C/N], or ratios that are modified by the Galactic chemical evolution, such as [Y/Mg], [Y/Al] etc. In this talk, we aim at describing our method to calibrate empirical relations between abundance ratios, metallicity and stellar ages, using stars with asteroseismic ages (from the Kepler, K2 and TESS samples) present in the APOGEE, Gaia-ESO and GALAH surveys as calibrators. Finally, I will briefly show how high-quality spectra (HARPS-N@TNG and FIES@NOT) of a sample of 68 Kepler stars, for which we have precise ages from asteroseismology using individual mode frequencies, can enhance our ability to calibrate stellar age-chemistry relationships using chemical clocks. The orthogonal constraints offered by asteroseismic age, precise chemical compositions from ground-based high-resolution spectroscopy, and dynamics from the Gaia mission open the door to a more accurate understanding of the chemical evolution of the Galactic disk, tracing the processes of chemical enrichment with time.