SED template fits to HLS1-HLS9. The data points have been de-magnified according to our lensing models of the foreground cluster. These magnification factors can be found in Table 2. The solid lines show the best-fit R09 template (in blue) and CE01 template (in red) to the FIR-mm data, excluding the 24 m point. LABOCA 870 m and AzTEC 1.1 mm data are used to constrain these fits when the detection is of >3- significance. However, only the MIPS and Herschel data are shown in the figure. The dotted lines show the respective fits based solely on the observed 24 m point. Although both the R09 and the CE01 templates generally predict reasonable values for the IR luminosity based on observed 24 m emission, the 24 m-predicted SEDs typically do not provide reasonable fits to the FIR-mm data.

SED template fits to HLS10-HLS19. The data points have been de-magnified according to our lensing models of the foreground cluster. These magnification factors can be found in Table 2. The solid lines show the best-fit R09 template (in blue) and CE01 template (in red) to the FIR-mm data, excluding the 24 m point. LABOCA 870 m and AzTEC 1.1 mm data are used to constrain these fits when the detection is of >3- significance. However, only the MIPS and Herschel data are shown in the figure. The dotted lines show the respective fits based solely on the observed 24 m point. Although both the R09 and the CE01 templates generally predict reasonable values for the IR luminosity based on observed 24 m emission, the 24 m-predicted SEDs typically do not provide reasonable fits to the FIR-mm data.