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Aims. The aim of this work is the study of abundances of the heavy elementsBa, La, Ce, Nd, and Eu in 56 bulge giants (red giant branch and red clump) withmetallicities ranging from -1.3 dex to 0.5 dex. Methods. We obtainedhigh-resolution spectra of our giant stars using the FLAMES-UVES spectrographon the Very Large Telescope. We inspected four bulge fields along the minoraxis. Results. We measure the chemical evolution of heavy elements, as afunction of metallicity, in the Galactic bulge. Conclusions. The [Ba, La, Ce,Nd/Fe] vs. [Fe/H] ratios decrease with increasing metallicity, in which aspectthey differ from disc stars. In our metal-poor bulge stars, La and Ba areenhanced relative to their thick disc counterpart, while in our metal-richbulge stars La and Ba are underabundant relative to their disc counterpart.Therefore, this contrast between bulge and discs trends indicates that bulgeand (solar neighbourhood) thick disc stars could behave differently. Anincrease 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 tooperate at a metallicity around solar. Finally, [Eu/Fe] follows the[{\alpha}/Fe] behaviour, as expected, since these elements are produced by SNetype II.

Heavy elements Ba, La, Ce, Nd, and Eu in 56 Galactic bulge red giants