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The spatial distribution of elemental abundances in the disc of our Galaxygives insights both on its assembly process and subsequent evolution, and onthe stellar nucleogenesis of the different elements. Gradients can be tracedusing several types of objects as, for instance, (young and old) stars, openclusters, HII regions, planetary nebulae. We aim at tracing the radialdistributions of abundances of elements produced through differentnucleosynthetic channels -the alpha-elements O, Mg, Si, Ca and Ti, and theiron-peak elements Fe, Cr, Ni and Sc - by using the Gaia-ESO idr4 results ofopen clusters and young field stars. From the UVES spectra of member stars, wedetermine the average composition of clusters with ages >0.1 Gyr. We derivestatistical ages and distances of field stars. We trace the abundance gradientsusing the cluster and field populations and we compare them with achemo-dynamical Galactic evolutionary model. Results. The adoptedchemo-dynamical model, with the new generation of metallicity-dependent stellaryields for massive stars, is able to reproduce the observed spatialdistributions of abundance ratios, in particular the abundance ratios of [O/Fe]and [Mg/Fe] in the inner disc (5 kpc<RGC <7 kpc), with their differences, thatwere usually poorly explained by chemical evolution models. Often, oxygen andmagnesium are considered as equivalent in tracing alpha-element abundances andin deducing, e.g., the formation time-scales of different Galactic stellarpopulations. In addition, often [alpha/Fe] is computed combining severalalpha-elements. Our results indicate, as expected, a complex and diversenucleosynthesis of the various alpha-elements, in particular in the highmetallicity regimes, pointing towards a different origin of these elements andhighlighting the risk of considering them as a single class with commonfeatures.

The Gaia-ESO Survey: radial distribution of abundances in the Galactic disc from open clusters and young field stars