$N_{2rt}/N_{pt}$ of stars within the central part of the cluster, inside 2$r_t$ ($N_{2rt}$), to stars in the preceding tail ($N_{pt}$) is considerably higher for Praesepe than for the Hyades, namely 5 and 2, respectively. This may indicate a later stage of dynamical evolution of the Hyades. They may be closer to dissolution than is Praesepe. However, this hypothesis must be supported by future investigations, e.g. N-body simulations.

Summary {#summ}
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Using the data from Gaia DR2, we searched for the presence of Praesepe’s (NGC 2632) tidal tails in a sphere of some 400 pc radius around the Sun. First, the Gaia DR2 data were cleaned according to the recipes given in and described in Sec. \[prep\] to obtain an astrometrically and photometrically clean sample. Within this volume we cut a slice of $\pm$ 50 pc around the $Z_c$ coordinate of Praesepe and a primary window of 7 km s$^{-1}$ by 7 km s$^{-1}$ in velocity space around the expected tangential velocity of Praesepe members predicted by the convergent point method. We developed a method to find over-densities in a 5-D phase space with 3 spatial coordinates and 2 in velocity space. By modelling the Galactic background distribution via a Poisson 