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We have developed a model atom for Cu with which we perform statisticalequilibrium computations that allow us to compute the line formation of Cu Ilines in stellar atmospheres without assuming Local Thermodynamic Equilibrium(LTE). We validate this model atom by reproducing the observed line profiles ofthe Sun, Procyon and eleven metal-poor stars. Our sample of stars includes bothdwarfs and giants. Over a wide range of stellar parameters we obtain excellentagreement among different Cu I lines. The eleven metal-poor stars have ironabundances in the range -4.2 <= [Fe/H] <= -1.4, the weighted mean of the[Cu/Fe] ratios is -0.22 dex, with a scatter of -0.15 dex. This is verydifferent from the results from LTE analysis (the difference between NLTE andLTE abundances reaches 1 dex) and in spite of the small size of our sample itprompts for a revision of the Galactic evolution of Cu.

Galactic evolution of Copper in the light of NLTE computations