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Fig. 3


A plot of the ratio of the SFRs derived from the observed FUV or 24 μm fluxes over the SFRs derived from the da Cunha et al. (2008) model as a function of the model SFR. Red open circles and red open triangles are the SFRs derived from the MIPS 24 μm fluxes for early and the late-type galaxies respectively. Green open circles and green open triangles mark the estimates based on the FUV to IR excess as described by Buat et al. (2005). Filled blue triangles indicate late-type galaxies for which the SFRs are derived from the FUV after estimating the extinction using the β slope method of Meurer et al. (1999). The dashed line is the one-to-one relation. The histogram of the ratios for each method is indicated in the right panel.

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