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We examine whether the observed large $\sigma_{v}$ are the manifestation of external pressures necessary to keep the clouds in equilibrium. In Fig.\[fig:slw\]b, we plot the mass surface density ($\Sigma_{\rm H_2}$) against the ${\sigma_v}^2/r$ value of the KN clouds, along with those in the Milky Way from Heyer et al. (2009); in 30 Dor from Pineda et al. (2009) and Nayak et al. (2016); and in the LMC from Wong et al. (2011). Isolated virial clouds confined by self-gravity follow a linear relation in the ${\sigma_v}^2/r$ vs. $\Sigma_{\rm H_2}$ plot (for e.g. see Heyer et al. 2009). The values of clouds from the literature fall along this expectation. However, the KN clouds alone depart from the expected relation, and are likely confined by external pressure and not in virial equilibrium. Following the simplifying assumptions of Field et al. (2011), we plot isobars of external pressure (in terms of $P/k_{\rm B}$) according to their prescription. The lines reflect the external pressure necessary to confine clouds for a given ${\sigma_v}^2/r$ assuming clouds with a centrally concentrated internal density structure approximated by hydrostatic equilibrium. From Fig.\[fig:slw\]b, we see that external pressures of $\sim\,10^6$cm$^{-3}$K are necessary 