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The radial metallicity distribution in the Galactic thin disc represents acrucial constraint for modelling disc formation and evolution. Open clustersallow us to derive both the radial metallicity distribution and its evolutionover time. In this paper we perform the first investigation of the present-dayradial metallicity distribution based on [Fe/H] determinations in late typemembers of pre-main-sequence clusters. Because of their youth, these clustersare therefore essential for tracing the current inter-stellar mediummetallicity. We used the products of the Gaia-ESO Survey analysis of 12 youngregions (age<100 Myr), covering Galactocentric distances from 6.67 to 8.70 kpc.For the first time, we derived the metal content of star forming regionsfarther than 500 pc from the Sun. Median metallicities were determined throughsamples of reliable cluster members. For ten clusters the membership analysisis discussed in the present paper, while for other two clusters (Chamaeleon Iand Gamma Velorum) we adopted the members identified in our previous works. Allthe pre-main-sequence clusters considered in this paper have close-to-solar orslightly sub-solar metallicities. The radial metallicity distribution traced bythese clusters is almost flat, with the innermost star forming regions having[Fe/H] values that are 0.10-0.15 dex lower than the majority of the olderclusters located at similar Galactocentric radii. This homogeneous study of thepresent-day radial metallicity distribution in the Galactic thin disc favoursmodels that predict a flattening of the radial gradient over time. On the otherhand, the decrease of the average [Fe/H] at young ages is not easily explainedby the models. Our results reveal a complex interplay of several processes(e.g. star formation activity, initial mass function, supernova yields, gasflows) that controlled the recent evolution of the Milky Way.

The Gaia-ESO Survey: the present-day radial metallicity distribution of the Galactic disc probed by pre-main-sequence clusters