Notes. The whole spectroscopic catalogue is available at the CDS. P_prev is the probability assigned in the original article, while P_new is the probability derived in this work. Columns #3–#7 correspond to the dataset of B11 (heliocentric velocity, equivalent width of the Mg i line, metallicity, P_prev, P_new), while #8–#11 to the one of W09 (heliocentric velocity, pseudo-equivalent width of the Mg-triplet absorption feature, P_prev, P_new). With respect to the dataset of B11, the error in the equivalent width of the integrated fit of the Mg i line was updated from σ_EW = 2.8/(S/N) to σ_EW = 3.6/(S/N) (Battaglia & Starkenburg2012), while the metallicity and its error were derived as in B11, from the near-infrared Ca ii triplet (CaT) region adopting the calibration of Starkenburg et al. (2010). As B11 did not assign proper membership probabilities, just member and nonmember designation, we associated their members and nonmembers with membership probabilities of 1 and 0 respectively.