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Title: Multi-messenger Observations of a Binary Neutron Star Merger
Authors: Abbott, B. P
LIGO Scientific Collaboration
Fermi GBM
IceCube Collaboration
AstroSat Cadmium Zinc Telluride Imager Team
IPN Collaboration
The Insight-HXMT Collaboration
ANTARES Collaboration
The Swift Collaboration
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 Pathfinder
Las Cumbres Observatory Group
DWF ( Deeper, Wider, Faster Program )
CAASTRO Collaborations
The VINROUGE Collaboration
MASTER Collaboration
Caltech- NRAO
NuSTAR Collaborations
The MAXI Team
TZAC onsortium
KU Collaboration
Nordic Optical Telescope
Texas Tech University
SALT Group
TOROS: Transient Robotic Observatory of the South Collaboration
The BOOTES Collaboration
MWA: Murchison Widefield 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
Anupama, G. C
Pavana, M
Keywords: Gravitational waves;Stars: neutron
Issue Date: 20-Oct-2017
Publisher: IOP Publishing
Citation: The Astrophysical Journal Letters. Vol. 848, No. 2, L12
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 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 ˜ 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.
Description: Restricted Access
ISSN: 2041-8205
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Appears in Collections:IIAP Publications

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