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Fig. C.2

image

Dust mass abundances obtained fitting the SED of each region using 4 Myr ISRF and Desert dust model. Only fits with a are taken into account. The colour code is the same as in Fig. 5. Dot and dashed lines correspond to the values obtained by Paradis et al. (2011) for typical and bright H ii regions in the LMC modelled assuming a 4 Myr star cluster ISRF and Desert dust model.

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