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Fig. 5.
Fit to radio light curve of afterglow of GW170817 (Mooley et al. 2018a) in blue. The curve is plotted on a log-log scale to easily show the power-law dependence. The 3σ Apertif design sensitivity is shown in black. Three observations on the same days post merger as our observations for GW190425 are shown as orange stripes.
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