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The sigma Orionis cluster is to date the star-forming region with the largestnumber of confirmed brown dwarfs and substellar objects below the deuteriumburning mass limit. The most massive star, sigma Ori Aa, just in the clustercentre, is the \sim20Msol-mass O9.5V star that illuminates the HorseheadNebula, while the least massive object yet reported, S Ori 70, is only around 3MJup. In the middle, there is a continuum of stars and substellar objects ofall types (including magnetically active B2Vp stars, Herbig-Haro objects, FUOri stars or T Tauri brown dwarfs) that makes the cluster a cornerstone in thestudy of the initial mass function, disc presence, X-ray emission or accretionat all mass domains. However, the derived masses strongly depend on the actualheliocentric distance to the cluster. Gaia will solve the dilemma.

Gaia and sigma Orionis from 20 Msol to 3 MJup: the most complete and precise Initial Mass Function with a parallax determination?