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Fig. 7

image

Left column: comparison of A(Hα)24 μm, the attenuation of the Hα measured using different recipes based on the Hα over 24 μm flux ratio, and that determined using the Balmer decrement. Black symbols are for galaxies with σ [C(Hβ)] ≤ 0.1, red symbols for σ [C(Hβ)] > 0.1. Filled dots are for galaxies with a normal gas content (HI - def ≤ 0.4), empty symbols for gas-poor objects (HI - def > 0.4). The black solid lines show the 1:1 relation, the black long-dashed line the bisector fit determined using the best quality sample (σ [C(Hβ)] ≤ 0.1), while the red dotted line indicates the best fit determined using the whole sample. Right: comparison of A(Hα)24 μm and the attenuation A(FUV)24 μm determined in the GALEX FUV band using the prescription of Hao et al. (2011) based on the 24 μm emission band. The blue dotted-dashed line shows the relation expected for a screen model and the Galactic extinction law of Fitzpatrick & Massa (2007), the green short-dashed line the Calzetti attenuation law (Calzetti 2000), and the red dotted line the bisector fit to the data for all galaxies.

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