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Continued radio observations of GW170817 3.5 years post-merger
Using these results, we constrain the parameter space of models that predict a late-time radio re-brightening possibly arising from the high-velocity tail of the GW170817 kilonova ejecta, which would dominate the radio and X-ray emission years after the merger (once the structured jet afterglow fades below detection level).
High Energy Astrophysical Phenomena
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