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Gaia-ESO Survey observations of the young Gamma Velorum cluster led to thediscovery of two kinematically-distinct populations, Gamma Vel A and B,respectively, with population B extended over several square degrees in theVela OB2 association. Using the Gaia DR2 data for a sample of high-probabilitycluster members, we find that the two populations differ not onlykinematically, but are also located at different distances along the line ofsight, with the main cluster Gamma Vel A being closer. A combined fit of thetwo populations yields $\varpi_A = 2.895 \pm 0.008$ mas and $\varpi_B = 2.608\pm 0.017$ mas, with intrinsic dispersions of $0.038 \pm 0.011$ mas and $0.091\pm 0.016$ mas, respectively. This translates into distances of$345.4^{+1.0+12.4}_{-1.0-11.5}\,$ pc and $383.4^{+2.5+15.3}_{-2.5-14.2}\,$ pc,respectively, showing that Gamma Vel A is closer than Gamma Vel B by $\sim$38pc. We find that the two clusters are nearly coeval, and that Gamma Vel B isexpanding. We suggest that Gamma Vel A and B are two independent clusterslocated along the same line of sight.

The Gaia DR2 view of the Gamma Velorum cluster: resolving the 6D structure