Please use this identifier to cite or link to this item: https://hdl.handle.net/2440/111569
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 Type: Journal article Title: Multi-messenger observations of a binary neutron star merger Author: Abbott, B.Abbott, R.Abbott, T.Acernese, F.Ackley, K.Adams, C.Adams, T.Addesso, P.Adhikari, R.Adya, V.Affeldt, C.Afrough, M.Agarwal, B.Agathos, M.Agatsuma, K.Aggarwal, N.Aguiar, O.Aiello, L.Ain, A.Ajith, P.et al. Citation: Letters of the Astrophysical Journal, 2017; 848(2):L12-1-L12-59 Publisher: Institute of Physics Publishing Issue Date: 2017 ISSN: 2041-82052041-8213 Statement ofResponsibility: Roger W. Clay … Bruce R. Dawson … Miftar Ganija … Won Kim … James C. Lau … Jesper Munch … David J. Ottaway … Sally A. Robertson … Gavin P. Rowell … Peter J. Veitch … Fabien Voisin … et al. Abstract: On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s}}$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of ${40}_{-8}^{+8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 $\,{M}_{\odot }$. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc}}$) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta. Rights: Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. DOI: 10.3847/2041-8213/aa91c9 Grant ID: http://purl.org/au-research/grants/arc/FT150100099http://purl.org/au-research/grants/arc/FL150100148ARChttp://purl.org/au-research/grants/arc/CE170100013http://purl.org/au-research/grants/arc/CE1101020MOST104-2923-M-008-004-MY5MOST106-2112-M-008-007 Published version: http://dx.doi.org/10.3847/2041-8213/aa91c9 Appears in Collections: Aurora harvest 8Physics publications

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