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tokens: broadband SEDs, 19 with GROND and 3 with optical and NIR data from different instruments. For the rest of the GRBs at , we collected measurements from the literature if available; these measurements are listed in Table 3 . 4. Results The results, i.e., the best-fit models and parameters, from fitting the combined NIR, optical, and X-ray SEDs with the local extinction curves are summarized in the top portion of Table 2 and a plot containing all the SEDs is shown in Fig. 7 . As mentioned above, the SEDs of the 10 GRBs that show evidence for a small to medium amount of dust ( mag) were also fitted with the SN extinction curve. These SEDs are additionally plotted in Fig. 8 , in comparison to the best results from the local extinction curves (zoomed into the optical and NIR regime; the full plot is displayed in Fig. C.1 ). The corresponding parameters are given in the bottom portion of Table 2 . With these measurements we increase the number of determined values for GRBs at by a factor of 2–3. As previously observed for GRBs at lower redshift, the local extinction curves provide a good fit to the data, with the featureless SMC extinction curve usually best describing the observed magnitudes ( Greiner et al. 2011 ; Zafar et al. 2011a ). We find that from the 22 modeled GRBs at , 16 are best fit with the SMC and only 6 are best fit with the LMC or MW extinction curve. In contrast to other samples with GRBs at mostly , however, we find that all of the GRBs are only behind small to medium dust column densities ( mag) within their host galaxies line of sight, which is also true for the values collected from the literature (see Table 3 ). The distribution of our best-fit values compared to those from the unbiased samples from Greiner et al. (2011) and Covino et al. (2013) and the data from Zafar et al. (2011a) , based on the GRB sample from Fynbo et al. (2009) , is shown in Fig. 9 . While all of these samples include a % of GRBs with mag (and 3–5% with mag), only % of our GRBs at redshift have a visual extinction of mag and the remaining % have mag. A two-sample Kolmogorov-Smirnov test returns a rejection probability of % for the null hypothesis that the values from our GRBs at and those from Greiner et al. (2011) are drawn from the same sample. Considering the 10 SEDs that were also fitted with the SN extinction curve, we find that, besides GRB 090205 and 090516, the goodness of fit is comparable to the result from the local extinction curves, while for two of the bursts, GRB 140428A and 151027B, the SN extinction curve provides a better fit to the data. In case of GRB 140428A, the somewhat flat SED between the and band can be identified with the flattening between (rest-frame) 3000 and 1700 Å of the SN extinction curve () or as a small (rest-frame) 2175 Å feature when fitting the MW extinction curve (). This result is consistent with that from fitting the GROND SED to determine a photometric redshift, where we also find that the SN extinction curve is