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LIGO Scientific Collaboration (collab.), Virgo Collaboration (collab.), Pierre Auger Collaboration (collab.), et al., Hello Yann (collab.). (2017). Multi-messenger observations of a binary neutron star merger. Astrophysical Journal Letters, 848 (2), L12 [59 p.]. ISSN 2041-8205

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Lien direct chez l'éditeur doi:10.3847/2041-8213/aa91c9

Titre
Multi-messenger observations of a binary neutron star merger
Année de publication2017
Type de documentArticle référencé dans le Web of Science WOS:000413211000001
AuteursLIGO Scientific Collaboration (collab.), Virgo Collaboration (collab.), Pierre Auger Collaboration (collab.), et al., Hello Yann (collab.).
SourceAstrophysical Journal Letters, 2017, 848 (2), p. L12 [59 p.]. p. L12 [59 p.] ISSN 2041-8205
RésuméOn 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.
Plan de classementSciences de la Terre : généralités [060] ; Sciences fondamentales / Techniques d'analyse et de recherche [020] ; Limnologie physique / Océanographie physique [032]
LocalisationFonds IRD [F B010071328]
Identifiant IRDfdi:010071328
Lien permanenthttp://www.documentation.ird.fr/hor/fdi:010071328

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