members (candidates) for Praesepe and its tails. Henceforth we call this set of 1393 stars the Praesepe Sample (PrS). By adding $p_{cont}$ of the stars from the PrS we found a total contamination of 47 stars, 40 of which come from the stars in a 3-neighbourhood alone.

In Fig. \[Figure2\] we show the 1393 stars from Praesepe and its tails in the $(Y_P,X_P)$-plane and the $(Y_P,Z_P)$-plane. Stars coded in grey are 1266 stars with $p_{cont}$ &lt;0.015, in orange 53 stars with $p_{cont}$ $\approx$ 0.1 and in light green 74 stars with $p_{cont}$ $\approx$ 0.5. The tails extend up to 165 pc from the cluster centre. For comparison we also present the result of the N-body calculation for the Hyades cluster by , which we also transformed into the $X_P,Y_P,Z_P$ coordinate system of Praesepe. The model stars are shown as a beige density plot in the background. The coincidence between observations and model is remarkable, especially in the $(Y_P,X_P)$-plane. Such a good coincidence we already found in Paper I in the case of the Hyades. The present result could have been expected since the Hyades and Praesepe are very similar in age and in stellar content. Among the stars in Fig. 