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

TL;DR

This paper reports late-time optical and near-infrared observations of GW170817, revealing emission consistent with a structured relativistic jet interacting with the interstellar medium, challenging previous kilonova expectations.

Contribution

It provides new late-time observations that support a structured jet model over kilonova models for GW170817's afterglow.

Findings

Emission is brighter and bluer than kilonova models predict.

Data matches a Gaussian structured relativistic jet model.

Future observations will distinguish jet structure from cocoon models.

Abstract

The binary neutron star merger GW170817 was the first multi-messenger event observed in both gravitational and electromagnetic waves. The electromagnetic signal began approximately 2 seconds post-merger with a weak, short burst of gamma-rays, which was followed over the next hours and days by the ultraviolet, optical and near-infrared emission from a radioactively- powered kilonova. Later, non-thermal rising X-ray and radio emission was observed. The low luminosity of the gamma-rays and the rising non-thermal flux from the source at late times could indicate that we are outside the opening angle of the beamed relativistic jet. Alternatively, the emission could be arising from a cocoon of material formed from the interaction between a 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 post-merger. Our new observations are at odds with expectations of late-time emission from kilonova models, being too bright and blue. Instead, the emission arises from the interaction between the relativistic ejecta of GW170817 and the interstellar medium. We show that this emission matches the expectations of a Gaussian structured relativistic jet, which would have launched a high luminosity short GRB to an aligned observer. However, other jet structure or cocoon models can also match current data - the future evolution of the afterglow will directly distinguish the origin of the emission.