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Given the massive spectroscopic surveys and the Gaia mission, the Milky Wayhas turned into a unique laboratory to be explored using abundance ratios thatshow a strong dependency with time. Within this framework, the data providedthrough asteroseismology serve as a valuable complement. Yet, it has beendemonstrated that chemical traits can not be used as universal relations acrossthe Galaxy. To complete this picture, it is important to investigate thedependence on metallicity of the chemical ratios employed for inferring stellarages. We aim to explore different combinations of neutron-capture, odd-Z and$\alpha$ elements as a function of age, particularly focusing on theirmetallicity dependence for a sample of 74 giant field stars. Using UVESobservations, we derive atmospheric parameters and high-precision line by linechemical abundances (<0.04 dex) for the entire set of spectra. Stellar ages areinferred from astereoseismic information. By fitting chemical-age trends forthree different metallicity groups, we estimated their dependence onmetallicity. We found that the stronger chemical-age relations ([Zr/$\alpha$])are not necessarily the ratios with the smaller dependence on metallicity([Ce/$\alpha$] and [Ce/Eu]). We confirm the [n-capture/$\alpha$]-age trends forevolved stars, wherein the most significant correlation is evident in starswith solar-metallicity, gradually diminishing in stars with lower iron content.The lack of homogeneity within the metallicity range highlights the intricatenature of our Galaxy's star formation history and yield production. Metallicitydependence in s-process element yields and the impact of radial stellarmigration challenge the reliability of using chemical abundances alone to datestars. These discoveries raise doubts about universally valid chemical clocksapplicable across the entire Galaxy and its diverse metallicity ranges.

Exploring the dependence of chemical traits on metallicity: chemical trends for red giant stars with asteroseismic ages