Gaia-ESO Survey observations of the young Gamma Velorum cluster led to the discovery of two kinematically-distinct populations , Gamma Vel A and B , respectively , with population B extended over several square degrees in the Vela OB2 association . Using the Gaia DR2 data for a sample of high-probability cluster members , we find that the two populations differ not only kinematically , but are also located at different distances along the line of sight , with the main cluster Gamma Vel A being closer . A combined fit of the two 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 38 pc . We find that the two clusters are nearly coeval , and that Gamma Vel B is expanding . We suggest that Gamma Vel A and B are two independent clusters located along the same line of sight .