Section \[detect\] we describe the steps we took to find Praesepe’s tidal tails. Section \[detect\] is divided into subsections describing the cuts to obtain an astrometrically and photometrically clean sample, the separation of over-densities in position and velocity space from the Galactic background, the identification of Praesepe and its tails, and the estimation of contamination and completeness. In Section \[CAMDs\] we discuss the cluster and its tails and present some characteristic astrophysical parameters. A summary concludes the paper.

![image](Figure1a.pdf){width="\textwidth"}

![image](Figure1b.pdf){width="\textwidth"}

\

Finding Praesepe’s tidal tails {#detect}
==============================

The N-body simulations of the dynamical evolution of a Galactic open cluster literally were tailored to model the case of the Hyades cluster at an age of $\log \rm{t}$ = 8.8 [@2018ApJ...856...40M; @2018ApJ...863...67G] and at about the galacto-centric distance of the Sun. As the galacto-centric distance and age of Praesepe are comparable to that of the Hyades, and as the clusters are also similar with regard to their stellar content, it is justified that we use the data set of the model from as our model cluster to compare with the observations of Praesepe.

As a starting point we determined the 6-D phase space coordinates of the centre of Praesepe on the basis 