Upper panel: substellar IMF for the spectroscopically confirmed population of substellar members of the IC 348 cluster for a complete and extinction-limited sample of A_V ≤ 4 mag (red), and for the 16′  ×  14′ field from Luhman et al. (2003b) (black). The dotted line corresponds to the completeness limit of our survey. Lower panel: substellar IMF for the ρ Ophiuchi cluster (Alves de Oliveira et al. 2012), for two extinction-limited samples of A_V ≤ 8 mag (black) and A_V ≤ 15 mag (red). The best fit to a power law for masses  ≤80 M_Jup and the respective logarithmic exponent are shown².