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Multi-messenger Observations of a Binary Neutron Star Merger

2017-10-16Journal article Open access
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dc.contributor.authorPierre Auger and other collaborations (3541 authors)
dc.contributor.authorMura, G.La
dc.contributor.authorAbreu, P.
dc.contributor.authorAndringa, S.
dc.contributor.authorAssis, P.
dc.contributor.authorBlanco, A.
dc.contributor.authorCazon, L.
dc.contributor.authorConceição, R.
dc.contributor.authorDiogo, F.
dc.contributor.authorEspadanal, J.
dc.contributor.authorLopes, L.
dc.contributor.authorPimenta, M.
dc.contributor.authorSantos, E.
dc.contributor.authorSarmento, R.
dc.contributor.authorTomé, B.
dc.date.accessioned2019-02-05T15:17:05Z
dc.date.available2019-02-05T15:17:05Z
dc.date.issued2017-10-16
dc.date.updated2019-02-05T15:17:05Z
dc.description.abstractOn 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 deg(2) 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.
dc.description.versionPeer Reviewed
dc.identifierAstrophys.J. 848 (2017) L12 ApJL 848 L12 2017; DOI 10.3847/2041-8213/aa91c9
dc.identifier.urihttp://dx.doi.org/10.3847/2041-8213/aa91c9
dc.identifier.urihttp://hdl.handle.net/10400.26/27475
dc.language.isoeng
dc.titleMulti-messenger Observations of a Binary Neutron Star Merger
dc.typejournal article
dspace.entity.typePublication
rcaap.rightsopenAccesspt
rcaap.typearticle

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