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Fig. 5


70-to-100 versus 24-to-70 flux density ratios for each pixel at a resolution of 33 pc (left) and 260 pc (right). The colour of each symbol corresponds to ΣSFR, according to the colour bar on the right. The grid represents the models of Draine & Li (2007), with the MW3.1_30 dust composition, 0.10 ≤ Umin ≤ 25, and 0.00 ≤ γ ≤ 0.20. The red dashed lines indicate the locus corresponding to the one-to-one relations shown in Fig. 4. The 3σ uncertainties are shown in the bottom right corner. The 24-to-70 ratio is well correlated with γ and ΣSFR, especially at 33 pc. At 260 pc, due to mixing between diffuse and star-forming regions, excursions in γ are strongly reduced. Note that when considering the galaxy as a whole, a large part of the emission is due to the handful of luminous regions and not to the larger number of faint regions.

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