  Abundances of s-capture process elements in stars with exquisite
asteroseismic, spectroscopic, and astrometric constraints offer a novel
opportunity to study stellar evolution, nucleosynthesis, and Galactic chemical
evolution. We aim to investigate one of the least studied s-process elements in
the literature, Ce, using stars with asteroseismic constraints from the Kepler,
K2 and TESS missions. We combine the global asteroseismic parameters derived
from precise light curves obtained by the Kepler, K2 and TESS missions with
chemical abundances from the APOGEE DR17 survey and astrometric data from the
Gaia mission. Finally, we compute stellar ages using the code PARAM. We
investigate the different trends of [Ce/Fe] as a function of [Fe/H], [alpha/Fe]
and age considering the dependence on the radial position, specially in the
case of K2 targets which cover a large Galactocentric range. We, finally,
explore the [Ce/alpha] ratios as a function of age in different Galactocentric
intervals. The studied trends display a strong dependence of the Ce abundances
on [Fe/H] and star formation history. Indeed, the [Ce/Fe] ratio shows a
non-monotonic dependence on [Fe/H] with a peak around -0.2 dex. Moreover,
younger stars have higher [Ce/Fe] and [Ce/alpha] ratios than older stars,
confirming the latest contribution of low- and intermediate-mass asymptotic
giant branch stars to the Galactic chemical enrichment. In addition, the trends
of [Ce/Fe] and [Ce/alpha] with age become steeper moving towards the outer
regions of the Galactic disc, demonstrating a more intense star formation in
the inner regions than in the outer regions. Ce is thus a potentially
interesting element to help constraining stellar yields and the inside-out
formation of the Milky Way disc. However, the large scatter in all the
relations studied here, suggests that spectroscopic uncertainties for this
element are still too large.
