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Fig. 7


Attenuation in the FUV band versus the attenuation in Hα. The colour of each point indicates ΣSFR (upper row) or the sSFR (lower row), following the bar to the right. In the bottom row, the number of regions N and the Spearman correlation coefficient ρ are indicated. To compute the sSFR, the stellar mass in each region was computed from the 3.6 μm emission using the linear conversion factor of Zhu et al. (2010). The red line shows the one-to-one relation. The black, magenta, and cyan lines represent the attenuation for a starburst, a Milky Way, and an LMC average curve with differential reddening (fE(BV)continuum/E(BV)gas = 0.44, solid, with E(BV)continuum being the reddening between the V and B bands of the stellar continuum and E(BV)gas being that of the ionised gas) and without (f = 1, dashed). For the starburst relation, we assumed that even though the stellar continuum follows the starburst curve, the gas still follows a Milky Way curve. Note that the black and cyan solid lines are nearly overlap. At the finest resolution, there is a broad range in terms of differential reddening. Intense star-forming regions have little differential reddening, whereas diffuse regions present a strong differential reddening. On coarser scales, the averaging between diffuse and star-forming regions yields a differential reddening that is similar to that of starburst galaxies. The overall shape of the attenuation law is only weakly constrained, however, and may vary across the galaxy.

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