Online Material

Table 1: Flux densities measured from the MIPS and Herschel maps.

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{f3_14693.eps} \end{figure}$

Figure 3:

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 $\mu$ m point. LABOCA 870 $\mu$ m and AzTEC 1.1 mm data are used to constrain these fits when the detection is of >3- $\sigma$ 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 $\mu$ m point. Although both the R09 and the CE01 templates generally predict reasonable values for the IR luminosity based on observed 24 $\mu$ m emission, the 24 $\mu$ m-predicted SEDs typically do not provide reasonable fits to the FIR-mm data.

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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{f4_14693.eps} \end{figure}$

Figure 4:

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 $\mu$ m point. LABOCA 870 $\mu$ m and AzTEC 1.1 mm data are used to constrain these fits when the detection is of >3- $\sigma$ 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 $\mu$ m point. Although both the R09 and the CE01 templates generally predict reasonable values for the IR luminosity based on observed 24 $\mu$ m emission, the 24 $\mu$ m-predicted SEDs typically do not provide reasonable fits to the FIR-mm data.

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