Although the departure from the relation is not at the same scale as the KN clouds, this might still indicate that the observed $\sigma_{v}$–$r$ relation might be a function of distance from R136, and a more global property of 30Doradus.

The position of the KN molecular clouds in the $\sigma_{v}$–$r$ diagram implies either of two scenarios; the clouds are collapsing or expanding, or the observed line widths are the manifestation of external pressures that keep the clouds in equilibrium. Since collapse velocities are generally only $\sim40$% larger than equilibrium velocity dispersions for a self-gravitating cloud, the observed large linewidths for the sizes of the KN clouds are probably not the result of collapse (Ballesteros-Paredes et al. 2011). Neither are they likely to result from expansion because there is no obvious shell or hole structure that usually accompanies expansion.

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  Name               R.A.                       Dec.                $V_{\rm lsr}$   $\sigma_{\rm v}$      $L_{\rm CO}$            $r$           $M_{\rm H_2}$         $M_{\rm vir}$
                    (J2000)                   (J2000)               (kms$^{-1}$)      (kms$^{-1}$)     (Kkms$^{-1}$pc$^2$)       (pc)        (10$^3\,M_{\odot}$)   (10$^3\,M_{\odot}$)
  30Dor-KN1    5$^h$38$^m$45$^s$   $-$69$^{\rm \circ}$06$'$00$''$   237.2$\pm$0.1     4.0$\pm$0.7        154.2$\pm$21.3      3.93$\pm$0.58       2.7$\pm$0.2          10.9$\pm$3.3
  30Dor-KN2    5$^h$38$^m$40$^s$   $-$69$^{\rm \circ}$05$'$30$''$   244.4$\pm$0.2     4.4$\pm$0.1         243.6$\pm$3.7      3.35$\pm$0.5        4.2$\pm$0.3          11.25$\pm$1.8
  30Dor-KN3    5$^h$38$^m$36$^s$   $-$69$^{\rm \circ}$05$'$30$''$   250.0$\pm$0.2     5.0$\pm$0.3        320.8$\pm$44.3      2.96$\pm$0.44       5.3$\pm$0.4          12.83$\pm$2.5
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