Members of the Eulalia family from Walsh et al. (2013) in two-dimensional projections of the proper elements space: (i) semimajor axis a_P vs. eccentricity e_P (top); and (ii) semimajor axis a_P vs. inclination I_P (bottom). The star indicates location of 495 Eulalia, the suggested largest fragment in the family. Its very close proximity to the prominent mean motion resonance J3/1 (gray area) makes the proper eccentricity value unstable. On a timescale of tens to hundreds of Myr it can change by ~± 0.02, on occasions be aligned with the mean value in the family defined by members ejected onto safer orbits far from this resonance.