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We study the three dimensional arrangement of young stars in the solarneighbourhood using the second release of the Gaia mission (Gaia DR2) and weprovide a new, original view of the spatial configuration of the star formingregions within 500 pc from the Sun. By smoothing the star distribution througha gaussian filter, we construct three dimensional density maps for early-typestars (upper-main sequence, UMS) and pre-main sequence (PMS) sources. The PMSand the UMS samples are selected through a combination of photometric andastrometric criteria. A side product of the analysis is a three dimensional,G-band extinction map, which we use to correct our colour-magnitude diagram forextinction and reddening. Both density maps show three prominent structures,Scorpius-Centaurus, Orion, and Vela. The PMS map shows a plethora of lower massstar forming regions, such as Taurus, Perseus, Cepheus, Cassiopeia, andLacerta, which are less visible in the UMS map, due to the lack of largenumbers of bright, early-type stars. We report the finding of a candidate newopen cluster towards $l, b \sim 218.5^{\circ}, -2^{\circ}$, which could berelated to the Orion star forming complex. We estimate ages for the PMS sampleand we study the distribution of PMS stars as a function of their age. We findthat younger stars cluster in dense, compact clumps, and are surrounded byolder sources, whose distribution is instead more diffuse. The youngest groupsthat we find are mainly located in Scorpius-Centaurus, Orion, Vela, and Taurus.Cepheus, Cassiopeia, and Lacerta are instead more evolved and less numerous.Finally, we find that the three dimensional density maps show no evidence forthe existence of the ring-like structure which is usually referred to as theGould Belt.

3D mapping of young stars in the solar neighbourhood with Gaia DR2