@Article{LIGOSci_etal2017,
author="LIGO Sci, Virgo
and Barrios-Marti, J.
and Coleiro, A.
and Hernandez-Rey, J. J.
and Illuminati, G.
and Lotze, M.
and T{\"o}nnis, C.
and Zornoza, J. D.
and Zu{\~{n}}iga, J.",
title="Multi-messenger Observations of a Binary Neutron Star Merger",
journal="Astrophysical Journal Letters",
year="2017",
publisher="Iop Publishing Ltd",
volume="848",
number="2",
pages="L12 - 59pp",
optkeywords="gravitational waves; stars: neutron",
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 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{\textquoteright}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.",
optnote="WOS:000413211000001",
optnote="exported from refbase (https://references.ific.uv.es/refbase/show.php?record=3354), last updated on Mon, 19 Aug 2019 06:55:12 +0000",
issn="2041-8205",
doi="10.3847/2041-8213/aa91c9",
opturl="http://arxiv.org/abs/1710.05833",
opturl="https://doi.org/10.3847/2041-8213/aa91c9",
archivePrefix="arXiv",
eprint="1710.05833",
language="English"
}