A mildly relativistic wide-angle outflow in the neutron-star merger event GW170817

GW170817 was the first gravitational-wave detection of a binary neutron-star merger(1). It was accompanied by radiation across the electromagnetic spectrum and localized(2) to the galaxy NGC 4993 at a distance of 40 megaparsecs. It has been proposed that the observed gamma-ray, X-ray and radio emission is due to an ultra-relativistic jet being launched during the merger (and successfully breaking out of the surrounding material), directed away from our line of sight (off-axis)(3-6). The presence of such a jet is predicted from models that posit neutron-star mergers as the drivers of short hard-gamma-ray bursts(7,8). Here we report that the radio light curve of GW170817 has no direct signature of the afterglow of an off-axis jet. Although we cannot completely rule out the existence of a jet directed away from the line of sight, the observed gamma-ray emission could not have originated from such a jet. Instead, the radio data require the existence of a mildly relativistic wide-angle outflow moving towards us. This outflow could be the high-velocity tail of the neutron-rich material that was ejected dynamically during the merger, or a cocoon of material that breaks out when a jet launched during the merger transfers its energy to the dynamical ejecta. Because the cocoon model explains the radio light curve of GW170817, as well as the gamma-ray and X-ray emission (and possibly also the ultraviolet and optical emission)(9-15), it is the model that is most consistent with the observational data. Cocoons may be a ubiquitous phenomenon produced in neutron-star mergers, giving rise to a hitherto unidentified population of radio, ultraviolet, X-ray and gamma-ray transients in the local Universe.