the refinement of the membership list by removing candidates outside certain bands around the cluster main sequence as defined by theoretical evolutionary tracks. These cuts are also applied in other representation sub-spaces such as derived from radial velocity, spectral type, gravity, activity, metallicity, or lithium line measurements.

The aforecited work by [@2012MNRAS.422.1495L] and the companion articles [@2013MNRAS.431.3222L], [@2012MNRAS.426.3419B], and [@2012MNRAS.426.3403L], are recent examples of the classical methodology to derive membership lists from astro- and photometric data sets, this time in the same stellar cluster as studied in the current work: the Pleiades. [@2012MNRAS.422.1495L] defined the cluster sequence in the (Z-J)–Z CMD from previously known members; this sequence induces a conservative photometric cut in the original data set that is meant to remove a large part of field sources; finally, an initial list of membership probabilities is derived following an incorrect version[^1] of Eq. \[bayes.th\] applied to the VPD representation space. A threshold of $p=0.6$ results in 947 member candidates.

The methodologies presented thus far do not extend the probabilistic treatment first put forward by [@1958AJ.....63..387V] and for the VPD, to extended data sets with photometric or spectrometric measurements. An exception to this is the recent work by [@2013ApJ...762...88M] in young 