[X/Fe] vs. [Fe/H] trends (LTE) of the examined bulge giants: green squares denote stars with spectra having a S/N above 20, while the green empty circles denote stars having spectra with an S/N ≤ 20. The solid lines represent the running means and shaded areas show the 1σ scatter (only for stars with S/N > 20). The typical uncertainties for each element from Table 2 are also shown. In the plots we use A(Sc)_⊙ = 3.04 (Pehlivan Rhodin et al. 2017), A(V)_⊙ = 3.89, A(Cr)_⊙ = 5.62, A(Mn)_⊙ = 5.42, A(Fe)_⊙ = 7.47, A(Co)_⊙ = 4.93, and A(Ni)_⊙ = 6.20 (Scott et al. 2015). For spectra with S/N ≤ 20 the uncertainty in [X/Fe] becomes significantly large (see Jönsson et al. 2017a).