Multi-messenger observations of a binary neutron star merger

@article{Collaboration2017MultimessengerOO,
  title={Multi-messenger observations of a binary neutron star merger},
  author={Ligo Scientific Collaboration and Virgo Collaboration and Fermi Gbm and Integral and IceCube collaboration and AstroSat Cadmium Zinc Telluride Imager Team and Ipn Collaboration and The Insight-Hxmt Collaboration and Antares Collaboration and The Swift Collaboration and Agile Team and The Maxi Team and The Dark Energy Science Collaboration and The Des Collaboration and The DLT40 Collaboration and Grawita GRAvitational Wave Inaf TeAm and The Event Horizon Telescope Collaboration and Atca Australia Telescope Compact Array and A Pathfinder and Las Cumbres Observatory Group and OzGrav and Dwf and AST3 and Caastro Collaborations and The Vinrouge Collaboration and Master Collaboration and J-GEM and Growth and Jagwar and Caltech- Nrao and TTU-NRAO and NuSTAR collaborations and Pan-Starrs and The Maxi Team and Tzac Consortium and KU Collaboration and Nordic Optical Telescope and ePESSTO and Grond and Texas Tech University and Salt Collaborative Group and Toros Transient Robotic Observatory of the South Collaboration and The Bootes Collaboration and Mwa Murchison Widefield Array and The Calet Collaboration and IKI-GW Follow-up Collaboration and Hawc collaboration and Lofar Collaboration and Lwa Long Wavelength Array and Hawc collaboration and The Pierre Auger Collaboration and Almasop collaboration and Euro Vlbi Team and Pi of the Sky Collaboration and The Chandra Team at McGill University and Dfn Desert Fireball Network and Atlas and High Time Resolution Universe Survey and Rimas and Ratir and Ska South AfricaMeerKAT},
  journal={The Astrophysical Journal},
  year={2017},
  volume={848},
  pages={1-59}
}
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… 
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References

SHOWING 1-10 OF 155 REFERENCES
GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral.
TLDR
The association of GRB 170817A, detected by Fermi-GBM 1.7 s after the coalescence, corroborates the hypothesis of a neutron star merger and provides the first direct evidence of a link between these mergers and short γ-ray bursts.
GW170814: A Three-Detector Observation of Gravitational Waves from a Binary Black Hole Coalescence.
TLDR
For the first time, the nature of gravitational-wave polarizations from the antenna response of the LIGO-Virgo network is tested, thus enabling a new class of phenomenological tests of gravity.
Properties of the Binary Black Hole Merger GW150914.
TLDR
The data around the time of the event were analyzed coherently across the LIGO network using a suite of accurate waveform models that describe gravitational waves from a compact binary system in general relativity.
A radio counterpart to a neutron star merger
TLDR
Radio observations constrain the energy and geometry of relativistic material ejected from a binary neutron star merger, and the detection of a counterpart radio source that appears 16 days after the event is reported, allowing us to diagnose the energetics and environment of the merger.
GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2.
TLDR
The magnitude of modifications to the gravitational-wave dispersion relation is constrain, the graviton mass is bound to m_{g}≤7.7×10^{-23}  eV/c^{2} and null tests of general relativity are performed, finding that GW170104 is consistent with general relativity.
Insight-HXMT observations of the first binary neutron star merger GW170817
Finding the electromagnetic (EM) counterpart of binary compact star merger, especially the binary neutron star (BNS) merger, is critically important for gravitational wave (GW) astronomy, cosmology
A gravitational-wave standard siren measurement of the Hubble constant
TLDR
A measurement of the Hubble constant is reported that combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using the electromagnetic data.
Optical emission from a kilonova following a gravitational-wave-detected neutron-star merger
TLDR
Optical to near-infrared observations of a transient coincident with the detection of the gravitational-wave signature of a binary neutron-star merger and with a low-luminosity short-duration γ-ray burst are reported.
GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence.
TLDR
This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.
Detectable radio flares following gravitational waves from mergers of binary neutron stars
TLDR
Results of calculations are presented showing that the interaction of mildly relativistic outflows with the surrounding medium produces radio flares with peak emission at 1.4 gigahertz that persist at detectable (submillijansky) levels for weeks, out to a redshift of 0.1.
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