We modelled the distribution of examples of both members and non-members in several representation spaces discussed below. For example, a representation space can be composed of the two proper motions, and a subset of magnitudes and colour indices. These are the variables used to represent each source. In all cases, the likelihood model was derived only from complete observations, that is, from sources that have measurements available for all variables defining the representation space. This likelihood model was then used in Eq. \[bayes.th\] to infer the membership probabilities of all sources in the DANCe Pleiades data set.

We did not include in this likelihood model the spatial distribution of cluster members in the celestial sphere. This is because one of the main objectives of the analysis of the Pleaides DANCe dataset is to infer this spatial distribution and study the statistical significance of potential dependencies on the stellar mass. Thus, we prefered to not assume any model for the cluster members spatial density, and derived membership probabilities only from proper motions and colour-magnitude diagrams. We postpone the inclusion of the spatial information until a detailed analysis of the physical properties of the cluster members is carried out and made public 