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Multi-messenger observations of a binary neutron star merger
LIGO Scientific Collaboration and Virgo Collaboration; Fermi GBM; INTEGRAL; IceCube Collaboration; AstroSat Cadmium Zinc Telluride Imager Team; IPN Collaboration; The Insight-HXMT Collaboration; ANTARES Collaboration; The Swift Collaboration; AGILE Team; The 1M2H Team; The Dark Energy Camera GW-EM Collaboration and the DES Collaboration; The DLT40 Collaboration; GRAWITA: GRAvitational Wave Inaf TeAm; The Fermi Large Area Telescope Collaboration; ATCA: Australia Telescope Compact Array; ASKAP: Australian SKA Path finder; Las Cumbres Observatory Group; OzGrav; DWF (Deeper, Wider, Faster Program); AST3; CAASTRO Collaborations; The VINROUGE Collaboration; MASTER Collaboration; J-GEM; GROWTH; JAGWAR; Caltech- NRAO; TTU-NRAO; NuSTAR Collaborations; Pan-STARR; The MAXI Team; TZAC Consortium; KU Collaboration; Nordic Optical Telescope; ePESSTO; GROND; Texas Tech University; SALT Group; TOROS: Transient Robotic Observatory of the South Collaboration; The BOOTES Collaboration; MWA: Murchison Wide field Array; The CALET Collaboration; IKI-GW Follow-up Collaboration; H.E.S.S. Collaboration; LOFAR Collaboration; LWA: Long Wavelength Array; HAWC Collaboration; The Pierre Auger Collaboration; ALMA Collaboration; Euro VLBI Team; Pi of the Sky Collaboration; The Chandra Team at McGill University; DFN: Desert Fireball Network; ATLAS; High Time Resolution Universe Survey; RIMAS and RATIR; SKA South Africa / MeerKAT (2017). Multi-messenger observations of a binary neutron star merger. Astrophys. J. Lett. 848(2): L12.
In: The Astrophysical Journal: Letters. IOP Publishing: London. ISSN 2041-8205; e-ISSN 2041-8213, meer
Peer reviewed article  

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Author keywords
    gravitational waves; stars: neutron

Auteurs  Top 
  • LIGO Scientific Collaboration and Virgo Collaboration
  • Fermi GBM
  • IceCube Collaboration
  • AstroSat Cadmium Zinc Telluride Imager Team
  • IPN Collaboration
  • The Insight-HXMT Collaboration
  • ANTARES Collaboration
  • The Swift Collaboration
  • AGILE Team
  • The 1M2H Team
  • The Dark Energy Camera GW-EM Collaboration and the DES Collaboration
  • The DLT40 Collaboration
  • GRAWITA: GRAvitational Wave Inaf TeAm
  • The Fermi Large Area Telescope Collaboration
  • ATCA: Australia Telescope Compact Array
  • ASKAP: Australian SKA Path finder
  • Las Cumbres Observatory Group
  • OzGrav
  • DWF (Deeper, Wider, Faster Program)
  • AST3
  • CAASTRO Collaborations
  • The VINROUGE Collaboration
  • MASTER Collaboration
  • J-GEM
  • Caltech- NRAO
  • NuSTAR Collaborations
  • Pan-STARR
  • The MAXI Team
  • TZAC Consortium
  • KU Collaboration
  • Nordic Optical Telescope
  • Texas Tech University
  • SALT Group
  • TOROS: Transient Robotic Observatory of the South Collaboration
  • The BOOTES Collaboration
  • MWA: Murchison Wide field Array
  • The CALET Collaboration
  • IKI-GW Follow-up Collaboration
  • H.E.S.S. Collaboration
  • LOFAR Collaboration
  • LWA: Long Wavelength Array
  • HAWC Collaboration
  • The Pierre Auger Collaboration
  • ALMA Collaboration
  • Euro VLBI Team
  • Pi of the Sky Collaboration
  • The Chandra Team at McGill University
  • DFN: Desert Fireball Network
  • High Time Resolution Universe Survey
  • SKA South Africa / MeerKAT

    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.

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