Adelaide family represented by two possible plane-projections of proper orbital elements: (i) semi-major axis a_P vs. sine of inclination sinI_P (top panel), and (ii) semi-major axis a_P vs. eccentricity e_P (bottom panel). Shown are the largest fragment (525) Adelaide (diamond) and the smaller family members (black filled circles for multi-opposition orbits, grey for single-opposition orbits). The vertical and horizontal bars are the formal uncertainty values of the proper elements from Table A.1. The vertical grey stripes indicate the locations of several weak mean motion resonances (from left to right): 14J+9S-5, 8J+2E-9, and 15J-11S-3; the width of the line approximates resonances strength at the value of proper eccentricity using Gallardo (2014). Boxes A and B contain asteroids whose orbits are well separated from (525) Adelaide, suitable for dating family origin using backward integrations (see Sect. 2.4). The grey arrow in the top panel gives an estimate of maximum drift in semi-major axis of a ≃ 0.5 km asteroid, typical of many small members in the family (Fig. 4), in 500 kyr. The grey dashed ellipses indicate proper element zones in which fragments may land if ejected from (525) Adelaide with 6 m s⁻¹ velocity (assuming true anomaly f = 90° and argument of perihelion such that ω + f = 0° at origin).