Multi-messenger Observations of a Binary Neutron Star Merger<sup>*</sup>

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<jats:title>Abstract</jats:title> <jats:p>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 <jats:italic>Fermi</jats:italic> Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of <jats:inline-formula> <jats:tex-math> <?CDATA $\sim 1.7\,{\rm{s}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>∼</mml:mo> <mml:mn>1.7</mml:mn> <mml:mspace width="0.25em" /> <mml:mi mathvariant="normal">s</mml:mi> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa91c9ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg<jats:sup>2</jats:sup> at a luminosity distance of <jats:inline-formula> <jats:tex-math> <?CDATA ${40}_{-8}^{+8}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>40</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>8</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>8</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa91c9ieqn2.gif" xlink:type="simple" /> </jats:inline-formula> 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 <jats:inline-formula> <jats:tex-math> <?CDATA $\,{M}_{\odot }$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mspace width="0.25em" /> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa91c9ieqn3.gif" xlink:type="simple" /> </jats:inline-formula>. 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 <jats:inline-formula> <jats:tex-math> <?CDATA $\sim 40\,{\rm{Mpc}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>∼</mml:mo> <mml:mn>40</mml:mn> <mml:mspace width="0.25em" /> <mml:mi mathvariant="normal">Mpc</mml:mi> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa91c9ieqn4.gif" xlink:type="simple" /> </jats:inline-formula>) 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 <jats:inline-formula> <jats:tex-math> <?CDATA $\sim 9$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>∼</mml:mo> <mml:mn>9</mml:mn> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa91c9ieqn5.gif" xlink:type="simple" /> </jats:inline-formula> and <jats:inline-formula> <jats:tex-math> <?CDATA $\sim 16$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>∼</mml:mo> <mml:mn>16</mml:mn> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa91c9ieqn6.gif" xlink:type="simple" /> </jats:inline-formula> 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 <jats:italic>r</jats:italic>-process nuclei synthesized in the ejecta.</jats:p>

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