  We use an improved wavelet analysis technique to reconstruct the $(U,V,W)$
velocity distribution for $\sim 250000$ stars from Gaia DR2, residing in the
solar neighborhood of $200$~pc. The 2D wavelet transforms for three bivariate
distributions $(U,V)$, $(U,W)$, and $(V,W)$ were investigated. Though most of
currently known (low-velocity) stellar moving groups are densely overlapped in
these diagrams, our analysis allowed to detect and disentangle about twenty
statistically significant 3D groups of stars with high velocities. Most of them
appear new. We also discuss the issue of correct noise thresholding in the
wavelet transform and highlight the importance of using a global rather than
local statistic for that. Using of a local significance measure may lead to an
overstated statistical confidence for individual patterns due to the effect of
multiple testing.
