Notes. To provide an idea of the statistics, we also list the total number of A and earlier stars (N_A+) and the total number of F, G, and K stars (N_FGK) in the tail per one simulation. We calculate the half-number radius for each of the group separately (r_h, A+ and r_h, FGK). The values in Cols. 2–5 are for the tail in total, i.e. without any contamination taken into account. Columns 6–9 list the fraction p_A+ of stars earlier than A, and p_FGK for F, G, and K stars together which are located above the contamination threshold for the Besançon model, which is n_tl ≈ 7 × 10⁻⁸ pc⁻³ for A stars, and n_tl ≈ 1 × 10⁻⁵ pc⁻³ for FGK stars. The half-number radius for both subgroups calculated for stars that are above the density threshold is denoted r_h, A+ and r_h, FGK. Columns 10–13 are the same as Cols. 6–9, but for the case of the higher contamination, i.e. HyPl stream and the Besançon model together. In this case, the contamination threshold is n_tl ≈ 2 × 10⁻⁵ pc⁻³ for A stars and earlier, and n_tl ≈ 3 × 10⁻⁵ pc⁻³ for F, G, and K stars. The contamination threshold for both the Besançon model and HyPl stream is taken for velocity |v_tl| ≲ 4 km s⁻¹ around the (U_pl,V_pl,W_pl) = (−4.7, −23.8, −8.9) km s⁻¹ velocity of the Pleiades. The results are averaged over 4 simulations for the more massive clusters, and over 13 simulations for the lower mass clusters.