Context : Manganese is mainly produced in type II SNe during explosive silicon burning , in incomplete Si-burning regions , and depends on several nucleosynthesis environment conditions , such as mass cut beween the matter ejected and falling back onto the remnant , electron and neutron excesses , mixing fallback , and explosion energy .
Manganese is also produced in type Ia SNe .

Aims : The aim of this work is the study of abundances of the iron-peak element Mn in 56 bulge giants , among which 13 are red clump stars .
Four bulge fields along the minor axis are inspected .
The study of abundances of Mn-over-Fe as a function of metallicity in the Galactic bulge may shed light on its production mechanisms .

Methods : High-resolution spectra were obtained using the FLAMES+UVES spectrograph on the Very Large Telescope .
The spectra were obtained within a program to observe 800 stars using the GIRAFFE spectrograph , together with the present UVES spectra .

Results : We aim at identifying the chemical evolution of manganese , as a function of metallicity , in the Galactic bulge .
We find [ Mn/Fe ] \sim -0.7 at [ Fe/H ] \sim -1.3 , increasing to a solar value at metallicities close to solar , and showing a spread around -0.7 \mathrel { \hbox { \raise 2.15 pt \hbox { $ < $ } \hbox to 0.0 pt { \lower 2.15 pt \hbox { $ \sim$% } } } } [ Fe/H ] \mathrel { \hbox { \raise 2.15 pt \hbox { $ < $ } \hbox to 0.0 pt { \lower 2.15 pt \hbox { $ \sim$% } } } } -0.2 , in good agreement with other work on Mn in bulge stars .
There is also good agreement with chemical evolution models .
We find no clear difference in the behaviour of the four bulge fields .
Whereas [ Mn/Fe ] vs. [ Fe/H ] could be identified with the behaviour of the thick disc stars , [ Mn/O ] vs. [ O/H ] has a behaviour running parallel , at higher metallicities , compared to thick disc stars , indicating that the bulge enrichment might have proceeded differently from that of the thick disk .

Conclusions :