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The young $\sigma$-Orionis cluster is an important location for understandingthe formation and evolution of stars, brown dwarfs, and planetary-mass objects.Its metallicity, although being a fundamental parameter, has not been welldetermined yet. We present the first determination of the metallicity of nineyoung late-type stars in $\sigma$-Orionis. Using the optical and near-infraredbroadband photometry available in the literature we derive the effectivetemperatures for these nine cluster stars, which lie in the interval 4300--6500K (1--3 \Msuno). These parameters are employed to compute a grid of syntheticspectra based on the code MOOG and Kurucz model atmospheres. We employ a$\chi^2$-minimization procedure to derive the stellar surface gravity andatmospheric abundances of Al, Ca, Si, Fe, Ni and Li, using multi-object opticalspectroscopy taken with WYFFOS+AF2 at at the William Herschel Telescope($\lambda/\delta\lambda\sim7500$). The average metallicity of the$\sigma$-Orionis cluster is [Fe/H] $ = -0.02\pm0.09\pm0.13$ (random andsystematic errors). The abundances of the other elements, except lithium, seemto be consistent with solar values. Lithium abundances are in agreement withthe "cosmic" $^7$Li abundance, except for two stars which show a $\log\epsilon(\mathrm{Li})$ in the range 3.6--3.7 (although almost consistent withinthe error bars). There are also other two stars with $\log\epsilon(\mathrm{Li})\sim 2.75$. We derived an average radial velocity of the$\sigma$-Orionis cluster of $28\pm4$km/s. The $\sigma$-Orionis metallicity isroughly solar.

Chemical abundances of late-type pre-main sequence stars in the $\sigma$-Orionis cluster