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Context. Recent studies have suggested that moving groups have a dynamic or"resonant" origin. Under this hypothesis, these kinematic structures become apowerful tool for studying the large-scale structure and dynamics of the MilkyWay. Aims. We aim to characterize these structures in the U-V-age-[Fe/H] spaceand establish observational constraints that will allow us to study theirorigin and evolution. Methods. We apply multiscale techniques -waveletdenoising (WD)- to an extensive compendium of more than 24000 stars in thesolar neighbourhood with the best available astrometric, photometric andspectroscopic data. Results. We confirm that the dominant structures in the U-Vplane are the branches of Sirius, Coma Berenices, Hyades-Pleiades and Hercules,which are nearly equidistant in this kinematic plane and show a negative slope.The abrupt drops in the velocity distribution are characterized. We find acertain dependence of these kinematic structures on Galactic position with asignificant change of contrast among substructures inside the branches. A largespread of ages is observed for all branches. The Hercules branch is detected inall subsamples with ages older than ~ 2 Gyr and the set of the other threebranches is well established for stars > 400 Myr. The age-metallicity relationof each branch is examined and the relation between kinematics and metallicityis studied. Conclusions. Not all of these observational constraints aresuccessfully explained by the recent models proposed for the formation of suchkinematic structures. Simulations incorporating stellar ages and metallicitiesare essential for future studies. The comparison of the observed and simulateddistributions obtained by WD will provide a physical interpretation of theexistence of the branches in terms of local or large-scale dynamics. [Abridged]

Origin and evolution of moving groups I. Characterization in the observational kinematic-age-metallicity space