@article{fdi:010071328,
  title = {{M}ulti-messenger observations of a binary neutron star merger},
  author = {{LIGO} {S}cientific {C}ollaboration and {V}irgo {C}ollaboration and {P}ierre {A}uger {C}ollaboration and et al. and {H}ello, {Y}ann},
  editor = {},
  language = {{ENG}},
  abstract = {{O}n 2017 {A}ugust 17 a binary neutron star coalescence candidate (later designated {GW}170817) with merger time 12:41:04 {UTC} was observed through gravitational waves by the {A}dvanced {LIGO} and {A}dvanced {V}irgo detectors. {T}he {F}ermi {G}amma-ray {B}urst {M}onitor independently detected a gamma-ray burst ({GRB} 170817{A}) with a time delay of similar to 1.7 s with respect to the merger time. {F}rom 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) {M}pc and with component masses consistent with neutron stars. {T}he component masses were later measured to be in the range 0.86 to 2.26 {M}-circle dot. {A}n extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient ({SSS}17a, now with the {IAU} identification of {AT} 2017gfo) in {NGC} 4993 (at similar to 40 {M}pc) less than 11 hours after the merger by the {O}ne-{M}eter, {T}wo {H}emisphere (1{M}2{H}) team using the 1 m {S}wope {T}elescope. {T}he optical transient was independently detected by multiple teams within an hour. {S}ubsequent observations targeted the object and its environment. {E}arly ultraviolet observations revealed a blue transient that faded within 48 hours. {O}ptical and infrared observations showed a redward evolution over similar to 10 days. {F}ollowing 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. {B}oth 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. {N}o ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. {T}hese observations support the hypothesis that {GW}170817 was produced by the merger of two neutron stars in {NGC}4993 followed by a short gamma-ray burst ({GRB} 170817{A}) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.},
  keywords = {gravitational waves ; stars: neutron},
  booktitle = {},
  journal = {{A}strophysical {J}ournal {L}etters},
  volume = {848},
  numero = {2},
  pages = {{L}12 [59 p.]},
  ISSN = {2041-8205},
  year = {2017},
  DOI = {10.3847/2041-8213/aa91c9},
  URL = {https://www.documentation.ird.fr/hor/fdi:010071328},
}