 south regions N159S and Region 23 have a very narrow (and low) range of radiation field intensities, with \[U$_{min}$, U$_{max}$\] ranges of \[3.8-4.8\] for Region 6, \[3.0-4.0\] for Region 23. As observed previously, the PAH fraction is very low in the H[ii]{} regions compared to the diffuse ISM around those regions.

Finally, we also estimate the H[i]{} mass in each aperture. Values are tabulated in Table \[SED\_model\_results\]. As mentioned previously, the value of the Galactic G/D is 157. The LMC having a lower metallicity, the G/D of the LMC should be higher than this value. We observe a large spread in the H[i]{}/D values from one region to another, and low ratios in H[ii]{} regions, which is not surprising. Indeed, the whole region being a very large molecular complex, the molecular gas is thus expected to be a significant fraction of the total gas mass in those regions as well. As previously mentioned, further investigations including CO observations for the whole complex will be investigated in a future paper.

SPIRE/LABOCA colour-colour diagram 
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Figure \[SPIRE\_LABOCA\_colour\] shows S$_{350}$/S$_{870}$ versus S$_{250}$/S$_{350}$. We remove the radio contamination from the LABOCA flux densities used in this plot. The different lines are colours obtained modelling single temperature modified blackbodies with an emissivity index of 2.5, 2, 1.5 and 1 and generated with temperatures ranging from 5 (left) to 70K (right). The bright star-forming regions have higher S$_{250}$/S$_{350}$, consistent with regions with higher temperature dust. They also show lower S$_{350}$/S$_{870}$ ratios. N158 (region 3), N159 (region 1) and N160 (region 2) thus present “flatter" submm slope than regions of the diffuse ISM (i.e. higher 870 [$\mu$m]{} flux density for a fixed 350 [$\mu$m]{} flux density). Region 5 does not appear in the diagram because of its very high 350-to-870 colour. Figure \[SED\_main\] (bottom panel) suggests that the 870 [$\mu$m]{} flux density we derive coul