Heavy elements Ba, La, Ce, Nd, and Eu in 56 Galactic bulge red giants
  Aims. The aim of this work is the study of abundances of the heavy elements
Ba, La, Ce, Nd, and Eu in 56 bulge giants (red giant branch and red clump) with
metallicities ranging from -1.3 dex to 0.5 dex. Methods. We obtained
high-resolution spectra of our giant stars using the FLAMES-UVES spectrograph
on the Very Large Telescope. We inspected four bulge fields along the minor
axis. Results. We measure the chemical evolution of heavy elements, as a
function of metallicity, in the Galactic bulge. Conclusions. The [Ba, La, Ce,
Nd/Fe] vs. [Fe/H] ratios decrease with increasing metallicity, in which aspect
they differ from disc stars. In our metal-poor bulge stars, La and Ba are
enhanced relative to their thick disc counterpart, while in our metal-rich
bulge stars La and Ba are underabundant relative to their disc counterpart.
Therefore, this contrast between bulge and discs trends indicates that bulge
and (solar neighbourhood) thick disc stars could behave differently. An
increase in [La, Nd/Eu] with increasing metallicity, for metal-rich stars with
[Fe/H] > 0 dex, may indicate that the s-process from AGB stars starts to
operate at a metallicity around solar. Finally, [Eu/Fe] follows the
[{\alpha}/Fe] behaviour, as expected, since these elements are produced by SNe
type II.
