Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/41298
Title: Multi-messenger Observations of a Binary Neutron Star Merger
Authors: Beardmore, Andrew P.
Evans, Philip A.
Osborne, Julian P.
Pagani, Claudio
Page, Kim
Higgins, Adam B.
Starling, Rhaana L.C.
O'Brien, Paul T.
Rosetti, Skye S.
First Published: 3-Oct-2017
Publisher: American Astronomical Society
Citation: Astrophysical Journal Letters, 2017, 848, pp. 12-12 (59)
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 ~1.7 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. 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 ~40 Mpc) less than 11 hours after the merger by the OneMeter, 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 ~9 and ~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.
DOI Link: 10.3847/2041-8213/aa91c9
ISSN: 2041-8205
eISSN: 2041-8213
Links: http://iopscience.iop.org/article/10.3847/2041-8213/aa91c9/meta
http://hdl.handle.net/2381/41298
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: Copyright © the authors,2017. This is an open-access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/3.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited.
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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