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tokens: code. We adopt the high- z edition, which includes the modeling in the radio bands, as well as the Lyman absorptions in the rest-frame UV from the intergalactic medium ( da Cunha et al. 2015 ). We plotted the best-fit models in Fig. 6 , along with the photometric measurements, and the fitting results of HYPERZ and those using the infrared templates. Fig. 6. UV-to-radio SEDs for each of our sample SMGs except ALESS66.1 for which the UV-to-NIR photometric measurements are contaminated by a foreground quasar Simpson et al. (2014) . Sources that are identified to host an AGN are marked with an asterisk after the ID. The measurements are plotted as black points and the best-fit models from MAGPHYS , HYPERZ , and the IR templates compiled by Swinbank et al. (2014) are plotted as gray, blue, and red curves, respectively. For clarity, we do not show the uncertainty, however, it is discussed in the text, including the fact that the IR luminosities that were estimated by the two methods are in agreement with each other within the uncertainty. The insets are zoom-ins in the OIR regime from 0.3 to 10 μ m in log–log scale. We find significant differences in higher L IR sources between the best-fit models of MAGPHYS and HYPERZ ; also, in all of these discrepant cases, the HYPERZ modeling provides a better fit with a lower χ 2 . We first compare the infrared luminosities estimated from the SED templates 8 and those from MAGPHYS . We confirm that both values are statistically consistent with each other in all sources. We then turn to A V in which we find significant differences in some sources. As seen in Fig. 6 , ALESS67.1, ALESS75.1, and AS2UDS412.0 appear to have different best-fit models in the UV-to-NIR regime, although the fit from HYPERZ shows better agreement with the data. Interestingly, in these three cases where the A V differ, the values obtained from MAGPHYS are all higher. We note that given the different assumptions of the attenuation curves in these two codes, the A V values from the UV-to-NIR regime should also ideally be deduced from MAGPHYS by turning off the fitting of the MIR-to-radio part. Unfortunately, the public version of MAGPHYS does not support this option. However, the fact that the A V values are in excellent agreement with each other in ALESS17.1 and AS2UDS292.0, which is as expected from a good match shown in Fig. 6 , suggests that the systematic difference between the A V values can be neglected. We also tried to homogenize the two codes by running the HYPERZ fitting that only uses the τ -decay SFHs that are similarly adopted by MAGPHYS , thus definitively removing the bursting SFH in our adopted method for HYPERZ . We find that the output values vary within uncertainties and the conclusions remain unchanged. Since stellar mass is not one of the direct outputs from HYPERZ, we estimated the stellar masses by converting the absolute magnitude, which is one of the outputs from HYPERZ based on some estimates of mass-to-light