in detail. Future high angular resolution integral field unit (IFU) nIR spectroscopy would help towards constraining this further, as shocked gas will likely be offset in velocity.

A picture of ionization fronts emerges, with the photodissociation region extincted from our line of sight by the cold molecular gas. These structures could resemble the dense “pillars” or structures observed in the galaxy in regions such as M16 and NGC3603 (Sankrit & Hester 2000), but are smaller in scale at $\sim$0.1–0.3pc, and in the 30 Doradus Nebula by Pellegrini et al. (2010). From the observed emission line imaging and CO(2-1) observations it appears that the clouds are being ionised on the backside. We are viewing the KN molecular clouds face on, and they are likely the tail of pillar-like structures (we refer the reader to Pound 1998 for a description of pillar morphology; or to Fig.7) with the ionized head pointing towards R136. The observed velocity line widths of the CO(2-1) line are then likely caused due to the velocity gradient between the head and tail of pillars (e.g. Pound 1998). Following the Bertoldi (1989) analytical theory of photoevaporating clouds, during photoevaporation clouds form a cometary structure similar to pillars. Neutral gas 