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Multi-messenger Observations of a Binary Neutron Star Merger
Linnéuniversitetet, Fakulteten för teknik (FTK), Institutionen för fysik och elektroteknik (IFE).ORCID-id: 0000-0002-2115-2930
Linnéuniversitetet, Fakulteten för teknik (FTK), Institutionen för fysik och elektroteknik (IFE). Stockholms universitet.
Linnéuniversitetet, Fakulteten för teknik (FTK), Institutionen för fysik och elektroteknik (IFE).ORCID-id: 0000-0001-6511-4330
Linnéuniversitetet, Fakulteten för teknik (FTK), Institutionen för fysik och elektroteknik (IFE). Université Paris Diderot, France.ORCID-id: 0000-0002-4710-2165
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Antal upphovsmän: 35272017 (Engelska)Ingår i: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 48, nr 2, artikel-id L12Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

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 similar to 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 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-circle dot. 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 similar to 40 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 similar to 10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position similar to 9 and similar to 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 NGC4993 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.

Ort, förlag, år, upplaga, sidor
Institute of Physics Publishing (IOPP), 2017. Vol. 48, nr 2, artikel-id L12
Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Forskningsämne
Fysik, Astropartikelfysik
Identifikatorer
URN: urn:nbn:se:lnu:diva-69675DOI: 10.3847/2041-8213/aa91c9ISI: 000413211000001OAI: oai:DiVA.org:lnu-69675DiVA, id: diva2:1172641
Tillgänglig från: 2018-01-10 Skapad: 2018-01-10 Senast uppdaterad: 2018-01-12Bibliografiskt granskad

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Becherini, YvonneFarnier, ChristianProkhorov, DmitryPunch, Michael

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Astrophysical Journal Letters
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