  We introduce a new method for stacking voids and deriving their profile that
greatly increases the potential of voids as a tool for precision cosmology.
Given that voids are highly non-spherical and have most of their mass at their
edge, voids are better described relative to their boundary rather than
relative to their centre, as in the conventional spherical stacking approach.
The boundary profile is obtained by computing the distance of each volume
element from the void boundary. Voids can then be stacked and their profiles
computed as a function of this boundary distance. This approach enhances the
weak lensing signal of voids, both shear and convergence, by a factor of two
when compared to the spherical stacking method. It also results in steeper void
density profiles that are characterised by a very slow rise inside the void and
a pronounced density ridge at the void boundary. The resulting boundary density
profile is self-similar when rescaled by the thickness of the density ridge,
implying that the average rescaled profile is independent of void size. The
boundary velocity profile is characterized by outflows in the inner regions
whose amplitude scales with void size, and by a strong inflow into the
filaments and walls delimiting the void. This new picture enables a
straightforward discrimination between collapsing and expanding voids both for
individual objects as well as for stacked samples.
