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Fig. 10


Comparison of the SED derived instantaneous SFRs with the observation derived total SFRs. On the left are the fits with unconstrained extinction and on the right the ones with energy conservation. Each SFH with variable SFR is plotted separately, and the colorbar indicates t/τ, in logarithmic scale. Top is rising, middle is delayed and bottom is declining SFHs. The solid line is the one-to-one relation and the dashed lines are positioned at ±0.2 dex of it, illustrating the threshold of tolerance for matching the LIR. We can see that for most of our sample, when extinction is a free parameter (left) the photometries are interpreted as weakly star-forming or having decreased SFRs in comparison with what the UV and IR-derived SFRs show (except the rising models that are equally distributed around the one-on-one relation). This is not the case in the energy conserving fits (right). All the rising models tightly reproduce the observed SFRs (as do the CSFR models). In the case of the declining and delayed models, there is an extra feature: a fraction of the energy conserving fits have SFRSED<SFRUV + IR, and a large t/τ ratio.

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