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Fig. 2

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FIR-derived properties of our PACS-detected LBGs at z ~ 3 (light green dots for galaxies in GOODS-North, dark green dots for galaxies in GOODS-South), and at z ~ 1 (orange open squares). The grey shaded zones represent the accessible areas with PACS at z ~ 3 for log (LUV/L) > 10.0, or for log (LUV/L) > 11.0, which represent the range of the rest-frame UV luminosity for LBGs at z ~ 3. In the bottom-left and bottom-right panels, blue open triangles represent the whole sample of LBGs at z ~ 3 in GOODS-South regardless of the detection in PACS. The patterns seen in the blue triangles are due to the sampling of the BC03 templates employed to fit the rest-frame UV-to-NIR SED. In the fourth panel, the red straight line is the linear fit to the whole population of LBGs at z ~ 3, and the red dashed line is a linear fit to the PACS-detected LBGs at z ~ 3. Upper left: dust attenuation as parametrized by the ratio between the total IR and rest-frame UV luminosities (Buat et al. 2005) as a function of the UV continuum slope. The relations of Meurer et al. (1999) for local SB and Boissier et al. (2007) for local normal SF galaxies are represented with dashed and continuous curves, respectively. We also plot the correction of Takeuchi et al. (2012) to the Meurer et al. (1999) relation with a dashed-dotted curve. Upper right: UV+IR-derived total SFR against SED-derived dust corrected total SFR. Solid line is the one-to-one relation. Bottom left: SFR versus stellar mass plane. The solid line is the main sequence (MS) of galaxies at z ~ 2 reported in Daddi et al. (2007); dashed and dashed-dotted lines are 4 and 10 times the MS and are employed to separate normal SF galaxies from SB (Rodighiero et al. 2011). Bottom right: sSFR versus stellar mass plane.

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