The differential (histogram; left-hand panel) and cumulative (solid line; right-hand panel) IMFs produced by combining the stars and brown dwarfs from the three calculations with the highest opacities. In total, there are 535 stars and brown dwarfs. The double hatched histogram denotes those objects that have stopped accreting (defined as accreting at a rate of less than 10⁻⁷ M_⊙ yr⁻¹), while those objects that are still accreting when the calculations were stopped are plotted using single hatching. The differential IMF is compared with the parameterizations of the observed IMF by Salpeter (1955), Kroupa (2001), and Chabrier (2005). The cumulative IMF is compared with the cumulative IMF (dashed line; right-hand panel) from the parametrization of the observed IMF by Chabrier (2005). The vertical dashed line marks the stellar/brown dwarf boundary. A Kolmogorov–Smirnov test shows the numerical IMF to be indistinguishable from Chabrier's parametrization of the IMF (there is a 9 per cent probability that the numerical IMF could have been drawn from Chabrier's fit to the observed IMF).