in the document `GAIA-C3-TN-LU-LL-124-01` which can be found on ESA’s webpage[^1]. In this concept UWE is scaled by a factor depending on the magnitude and colour of the source. The result is a re-normalised UWE, or RUWE, which needs only a single threshold of 1.4. Values for RUWE can be found at the service[^2] in table `gaiaDR2light`. All the other cuts are the same as in Paper I. We obtained an astrometrically and photometrically clean sample of 8,131,092 stars out of the original 43 million objects. The price for this cleaning is an incompleteness at the faint end of the magnitude distribution near $G$ = 18 mag and also near the parallax limit of 2.4 mas.

Constraining the range in space and velocity {#CVspace}
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In general, a cluster and its possible tidal tails reveal themselves as an over-density in position- and velocity-space. In the ideal case, we need observed space velocities for each star in a sample to identify stars co-moving with the Praesepe cluster. However, accurate radial velocities are lacking for the vast majority of stars. Therefore we had to rely on criteria that are solely based on their tangential velocities. This implies that we may detect stars 