Afterglow of a GRB 170817A-like jet compared to the archival SGRB data from Fong et al. (2015). The redshift and ISM density have been set equal to the medians of the Fong et al. (2015) sample, namely z = 0.46 and n = 5 × 10⁻³ cm⁻³. Each panel shows data from a different frequency range: radio (1.4 ≤ ν/GHz ≤ 93, bottom left-hand panel), UVOIR (mostly r filter ≈4.8 × 10¹⁴ Hz, bottom right-hand panel), and X-ray (1 keV ≈2.4 × 10¹⁷ Hz, top panel). Upper limits are shown by empty turquoise downward triangles, while detections are shown by thin lines of different colours, each connecting data from a single SGRB. In each panel, thick solid black lines represent the GRB 170817-like jet light curve as seen on-axis, dashed black lines show the light curve for an observer at the border of the core, while solid orange lines show the light curve for viewing angle θ_v = 15° which corresponds to the best-fit value for GRB 1708017A as given in Ghirlanda et al. (2019). The model light curves are computed for observer frequencies ν_obs = 6 GHz (radio), 4.8 × 10¹⁴ Hz (optical) and 2.4 × 10¹⁷ Hz (X-ray).