3 years ago

The optical afterglow of the short gamma-ray burst associated with GW170817.

E. Pian, A. Rowlinson, P. Jakobsson, D. J. Watson, A. S. Fruchter, C. C. Thöne, M. Im, A. J. Levan, T. Kangas, L. Izzo, N. R. Tanvir, J. D. Lyman, K. Wiersema, P. Sutton, J. Hjorth, C. Copperwheat, A. de Ugarte Postigo, J. P. U. Fynbo, G. P. Lamb, E. Palazzi, D. A. Perley, C. Gall, D. Steeghs, B. Gompertz, I. Mandel, S. Schulze, S. Kobayashi, P. A. Evans, R. A. M. J. Wijers, J. P. Osborne, B. Milvang-Jensen, P. O'Brien, Z. Cano, I. A. Steele, S. Rosswog, E. R. Stanway

The binary neutron star merger GW170817 was the first multi-messenger event observed in both gravitational and electromagnetic waves. The electromagnetic signal began ~ 2 seconds after the merger with a weak, short burst of gamma-rays, which was followed over the course of the next hours and days by the ultraviolet, optical and near-infrared emission from a radioactively-powered kilonova. The low luminosity of the gamma-rays and the rising radio and X-ray flux from the source at late times could indicate that we are viewing this event outside the opening angle of the beamed relativistic jet launched during the merger. Alternatively, the emission could be arising from a cocoon of material formed from the interaction between a (possibly choked) jet and the merger ejecta. Here we present late-time optical detections and deep near-infrared limits on the emission from GW170817 at 110 days after the merger. Our new observations are at odds with expectations of late-time emission from kilonova models, being too bright and blue. Instead, this late-time optical emission arises from the optical afterglow of GRB 170817A, associated with GW170817. This emission matches the expectations of a structured relativistic jet, that would have launched a high luminosity short GRB to an aligned observer. The distinct predictions for the future optical behaviour in the structured-jet and cocoon models will directly distinguish the origin of the emission.

Publisher URL: http://arxiv.org/abs/1801.02669

DOI: arXiv:1801.02669v2

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