getsf CMFs of the W43-MM2&MM3 ridge built for a different core catalog (a), under different assumptions of dust temperature and emissivity (b and c), and fit over a different mass range (d). The cumulative CMFs, their completeness levels, power-law fits, global 3 σ uncertainties (explained in Sect. 5.1), and the Salpeter slope of the canonical IMF are represented as in Fig. 5. Panel a: CMF derived from the core catalog of Paper V (Louvet et al., in prep.), itself obtained by getsf extraction in the original & cleanest images of W43-MM2 and W43-MM3, showing a similar but slightly shallower slope of α = 0.86 ± 0.04. Panel b: CMF obtained with a mean T_dust = 23 K dust temperature for all cores, instead of T_dust in Fig. D.3, displaying a similar but slightly shallower slope of α = −0.83 ± 0.03. Panel c: CMF derived assuming a linear relation for the dust opacity with core mass (see Sect. 5.2) showing a steeper slope of α = −1.02 ± 0.03. Panel d: fitting the CMF of Fig. 5a in the low- to intermediate-mass range, 0.8–16 M_⊙. This leads to a similar but slightly shallower slope of α = -0.89 ± 0.04.