Top: (M_G, (G − R_p)₀) color-magnitude diagram for 21 Gaia DR3 stars located within 30 pc of HD 159595 and having similar galactic space motion (Sect. A.3). Potential members of BPMG, UCL, and US are marked by filled diamonds, circles, and triangles, respectively. The color of the symbols indicates the membership probability. A star with a group membership probability of no more than 10% in any of these clusters is marked by a cross. Stars with Gaia ruwe >1.2 (possible binaries) are denoted with large squares. Empirical sequences of different ages are from Gagné et al. (2021). Bottom: Galactic space velocity differences (Δ_UVW) as a function of positional differences (Δ_HD159595) with respect to HD 159595 for 19 stars, found to be young from the above 21.