Abundance-age relations with red clump stars in open clusters
  Context: Precise chemical abundances coupled with reliable ages are key
ingredients to understand the chemical history of our Galaxy. Open Clusters
(OCs) are useful for this purpose because they provide ages with good
precision.
  Aims: The aim of this work is to investigate the relations of different
chemical abundance ratios vs age traced by red clump (RC) stars in OCs.
  Methods: We analyze a large sample of 209 reliable members in 47 OCs with
available high-resolution spectroscopy. We applied a differential line-by-line
analysis to provide a comprehensive chemical study of 25 chemical species. This
sample is among the largest samples of OCs homogeneously characterized in terms
of atmospheric parameters, detailed chemistry, and ages.
  Results: In our metallicity range (-0.2<[M/H]<+0.2) we find that while most
Fe-peak and alpha elements have flat dependence with age, the s-process
elements show decreasing trends with increasing age with a remarkable knee at 1
Gyr. For Ba, Ce, Y, Mo and Zr we find a plateau at young ages (< 1 Gyr). We
investigate the relations of all possible combinations among the computed
chemical species with age. We find 19 combinations with significant slopes,
including [Y/Mg] and [Y/Al]. The ratio [Ba/alpha] is the one with the most
significant correlations found.
  Conclusions: We find that the [Y/Mg] relation found in the literature using
Solar twins is compatible with the one found here in the Solar neighbourhood.
The age-abundance relations show larger scatter for clusters at large distances
(d>1 kpc) than for the Solar neighbourhood, particularly in the outer disk. We
conclude that these relations need to be understood also in terms of the
complexity of the chemical space introduced by the Galactic dynamics, on top of
pure nucleosynthetic arguments, especially out of the local bubble.
