2 times lower than the KN3 cloud. Under the assumption that the molecular clouds detected in CO(2-1) were initially all of similar densities, and photoionization from R136 alone is evaporating the molecular cloud, then KN1 must be closer to R136 (considering it as the only source of external photoionization) because the ionizing flux decreases to the inverse square with distance.

Line of sight distances
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Our main results concerning the detection of cold molecular gas near R136 suffers from possible projection effects. Although the cold molecular gas detected in the CO(2-1) observations lies within 2-14pc in projection of the R136 cluster, the actual distance may likely be further in the line of sight direction allowing for the clouds to possibly survive photoionisation. Chevance et al. (2016) analyse the physical distance of the CO gas in 30 Doradus to the stars, by comparing the incident radiation field on the gas modelled against fIR observations in fine structure lines of the emitted radiation field measured from the known massive star population. By comparing the luminosity of the photodissociation region (which forms the interface between the photoionizing radiation from the stars and the gas) against their predictions, they are able to constrain the 