The optical afterglow of GW170817 at one year post-merger

G. P. Lamb; J. D. Lyman; A. J. Levan; N. R. Tanvir; T. Kangas; A. S. Fruchter; B. Gompertz; J. Hjorth; I. Mandel; S. R. Oates; D. Steeghs; K. Wiersema

doi:10.3847/2041-8213/aaf96b

paper

The optical afterglow of GW170817 at one year post-merger

arXiv:1811.11491 · doi:10.3847/2041-8213/aaf96b

Abstract

We present observations of the optical afterglow of GRB\,170817A, made by the {\it Hubble Space Telescope}, between February and August 2018, up to one year after the neutron star merger, GW170817. The afterglow shows a rapid decline beyond $170$ ~days, and confirms the jet origin for the observed outflow, in contrast to more slowly declining expectations for `failed-jet' scenarios. We show here that the broadband (radio, optical, X-ray) afterglow is consistent with a structured outflow where an ultra-relativistic jet, with Lorentz factor $Γ ≳ 100$ , forms a narrow core ( $\sim 5^{\circ}$ ) and is surrounded by a wider angular component that extends to $\sim 1 5^{\circ}$ , which is itself relativistic ( $Γ ≳ 5$ ). For a two-component model of this structure, the late-time optical decline, where $F \propto t^{- α}$ , is $α = 2.20 \pm 0.18$ , and for a Gaussian structure the decline is $α = 2.45 \pm 0.23$ . We find the Gaussian model to be consistent with both the early $\sim 10$ days and late $≳ 290$ days data. The agreement of the optical light curve with the evolution of the broadband spectral energy distribution and its continued decline indicates that the optical flux is arising primarily from the afterglow and not any underlying host system. This provides the deepest limits on any host stellar cluster, with a luminosity $≲ 4000 L_{⊙} (M_{F606W} ≳ - 4.3)$ .

arXiv comment8 pages, 3 figures, accepted for publication in ApJL

The optical afterglow of GW170817 at one year post-merger

Abstract

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