have Gaussian shapes and the line widths are broader than the thermal line widths. It is a reasonable assumption to make that the line profiles are produced by turbulent motions of the gas inside the clouds (Solomon et al. 1987).

Figure\[fig:slw\]a displays the position of the KN clouds in the $\sigma_{v}$–$r$ diagram. Also shown are results from Heyer et al. (2009) summarising the canonical relation found for Galactic clouds of $\sigma_{v} = 0.72\,r^{0.5}$; and clouds in the 30 Doradus region (from Pineda et al. 2009; having a resolution of 43$\arcsec$; and from Nayak et al. (2016) having a resolution of 2$\arcsec$), and in the LMC (excluding 30 Doradus) from Wong et al. (2011) whose study had a spatial resolution of 45$\arcsec$. Note that the Pineda et al. (2009) and Nayak et al. (2016) clouds do not cover the central region of 30 Doradus near R136, and there are no spatial overlaps between the KN clouds and the clouds they identify. The molecular clouds associated with the stapler nebula lie above the canonical $\sigma_{v}$–$r$ relation for Galactic clouds. Interestingly, the other detected clouds in 30Doradus from Pineda et al. (2009) and Nayak et al. (2016) also lie above the canonical relation. 