Top panel: Relation graph between M_clump and M_vir. The dashed black line indicates the M_clump = M_vir relation. Middle panel: Clump mass as a function of radius for clumps. The grey area indicates the extent of the low-mass star-forming region. The dotted grey line indicates the threshold for the high-mass star formation M(r) 870 ≥ M_⊙ (r · pc⁻¹)^1.33 determined by Kauffmann & Pillai (2010). The dotted black line indicates the threshold (0.05 g cm⁻²) for the high-mass star formation determined by Urquhart et al. (2014b). The solid blue and green lines at the bottom right represent surface density thresholds for ‘efficient’ star formation of 116 M⊙ · pc⁻² [0.024 (g ·cm⁻²)](La et al. 2010; Lombardi et al. 2015) and 129 M_⊙ · pc⁻² 0.027 g · cm⁻² (Heiderman et al. 2010). In the plot, data points for clumps are depicted as black stars. Bottom panel: Non-thermal velocity dispersion σ_NT vs gas kinetic temperature derived from NH₃ (1,1) and (2,2).