Multi-messenger Observations of a Binary Neutron Star Merger

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dc.identifier.uri Adya, V.B. Affeldt, Christoph Allen, B. Ashton, G. Aulbert, C. Beer, C. Bergmann, G. Birnholtz, O. Bock, O. Bode, N. Brinkmann, M. Cabero, M. Capano, C.D. Danilishin, S.L. Danzmann, K. Denker, T. Dent, T. de Varona, O. Doravari, S. Drago, M. Dreissigacker, C. Fehrmann, H. Grote, H. Hanke, M.M. Heurs, M. Hu, Y.M. Indik, N. Junker, J. Karvinen, K.S. Khan, S. Kirchhoff, R. Koch, P. Koehlenbeck, S.M. Krämer, C. Kringel, V. Krishnan, B. Kuehn, G. et al. LIGO Scientific Collaboration Virgo Collaboration 2021-07-07T06:57:34Z 2021-07-07T06:57:34Z 2017
dc.identifier.citation Adya, V.B.; Affeldt, C.; Allen, B.; Ashton, G.; Aulbert, C. et al.: Multi-messenger Observations of a Binary Neutron Star Merger. In: The astrophysical journal : Part 2. Letters 848 (2017), Nr. 2, L12. DOI:
dc.description.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 ~ 1.7s 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 Mʘ. 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 ~40Mps) 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. eng
dc.language.iso eng
dc.publisher London : Institute of Physics Publ.
dc.relation.ispartofseries The astrophysical journal : Part 2. Letters 848 (2017), Nr. 2
dc.rights CC BY 3.0 Unported
dc.subject gravitational waves–stars: neutron eng
dc.subject binary neutron star coalescence candidate eng
dc.subject GW170817 eng
dc.subject Advanced LIGO eng
dc.subject Advanced Virgo eng
dc.subject Fermi Gamma-ray Burst Monitor eng
dc.subject.ddc 520 | Astronomie, Kartographie ger
dc.title Multi-messenger Observations of a Binary Neutron Star Merger
dc.type article
dc.type Text
dc.relation.essn 2041-8213
dc.relation.issn 2041-8205
dc.bibliographicCitation.issue 2
dc.bibliographicCitation.volume 848
dc.bibliographicCitation.firstPage L12
dc.description.version publishedVersion
tib.accessRights frei zug�nglich

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