Fig. 3.
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Dust luminosities estimated for the IR-detected sub-sample (592 galaxies out of 1049), with and without IR data. The solid black line shows the one-to-one relation. The dashed red line shows the best fit of this comparison, and ρ is the Pearson coefficient. The scatter is color-coded with the fluxes of the sub-sample at 250 μm.
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