Comparison of the prestellar CMFs (in ΔN/Δlog M format) expected in the toy model described in the text (solid curves) with the prestellar CMFs observed in the Orion B cloud complex (data points and histograms, adapted from Könyves et al. 2019) at low column densities (4 <   <  7.5, in blue), higher column densities (7.5 <   <  21, in red), and overall (all , in black). The black dotted line displays the Salpeter-like power law FLMF, dN/dlog , assumed in the toy model and consistent with the observed FLMF in the supercritical regime (see Fig. 1). The green dashed curve shows the system IMF (Chabrier 2005, see also Kroupa 2001). The two vertical dashed lines mark the estimated 80% completeness limits of the Herschel census of prestellar cores in Orion B at low and high background column densities respectively (see Könyves et al. 2019). The CMF extends to higher masses at higher column densities, i.e., higher M_line filaments in both the toy model and the observations.