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Aims. We aim to derive the chemical pattern of the young clusters 25 Orionisand lambda Orionis through homogeneous and accurate measurements of elementalabundances. Methods. We present FLAMES/UVES observations of a sample of 14K-type targets in the 25 Ori and lambda Ori clusters; we measure their radialvelocities, in order to confirm cluster membership. We derive stellarparameters and abundances of Fe, Na, Al, Si, Ca, Ti, and Ni using the codeMOOG. Results. All the 25 Ori stars are confirmed cluster members withoutevidence of binarity; in lambda Ori we identify one non-member and onecandidate single-lined binary star. We find an average metallicity[Fe/H]=-0.05+/-0.05 for 25 Ori, where the error is the 1sigma standarddeviation from the average. lambda Ori members have a mean iron abundance valueof 0.01+/-0.01. The other elements show close-to-solar ratios and nostar-to-star dispersion. Conclusions. Our results, along with previousmetallicity determinations in the Orion complex, evidence a small butdetectable dispersion in the [Fe/H] distribution of the complex. This appearsto be compatible with large-scale star formation episodes and initialnon-uniformity in the pre-cloud medium. We show that, as expected, theabundance distribution of star forming regions is consistent with the chemicalpattern of the Galactic thin disk.

Elemental abundances of low-mass stars in the young clusters 25 Ori and lambda Ori