  Using new proper motion data from recently published catalogs, we revisit the
membership of previously identified members of the Upper Scorpius association.
We confirmed 750 of them as cluster members based on the convergent point
method, compute their kinematic parallaxes and combined them with Gaia
parallaxes to investigate the 3D structure and geometry of the association
using a robust covariance method. We find a mean distance of $146\pm 3\pm 6$~pc
and show that the morphology of the association defined by the brightest (and
most massive) stars yields a prolate ellipsoid with dimensions of
$74\times38\times32$~pc$^{3}$, while the faintest cluster members define a more
elongated structure with dimensions of $98\times24\times18$~pc$^{3}$. We
suggest that the different properties of both populations is an imprint of the
star formation history in this region.
