TY - JOUR
T1 - Multi-messenger observations of a binary neutron star merger
AU - LIGO Scientific Collaboration and Virgo Collaboration
AU - Fermi GBM
AU - INTEGRAL
AU - Icecube Collaboration
AU - AstroSat Cadmium Zinc Telluride Imager Team
AU - IPN Collaboration
AU - Insight-HXMT Collaboration
AU - ANTARES Collaboration
AU - The Swift Collaboration
AU - AGILE Team
AU - 1M2H Team
AU - Dark Energy Camera GW-EM Collaboration and the DES Collaboration
AU - DLT40 Collaboration
AU - GRAWITA: GRAvitational Wave Inaf TeAm
AU - Fermi Large Area Telescope Collaboration
AU - ATCA: Australia Telescope Compact Array
AU - ASKAP: Australian SKA Pathfinder
AU - Las Cumbres Observatory Group
AU - OzGrav, DWF (Deeper, Wider, Faster program), AST3, and CAASTRO Collaborations
AU - VINROUGE Collaboration
AU - MASTER Collaboration
AU - J-GEM
AU - GROWTH, JAGWAR, Caltech-NRAO, TTU-NRAO, and NuSTAR Collaborations
AU - Pan-STARRS
AU - MAXI Team
AU - TZAC Consortium
AU - KU Collaboration
AU - Nordic Optical Telescope
AU - ePESSTO
AU - GROND
AU - Texas Tech University
AU - SALT Group
AU - TOROS: Transient Robotic Observatory of the South Collaboration
AU - BOOTES Collaboration
AU - MWA: Murchison Widefield Array
AU - CALET Collaboration
AU - IKI-GW Follow-up Collaboration
AU - H.E.S.S. Collaboration
AU - LOFAR Collaboration
AU - LWA: Long Wavelength Array
AU - HAWC Collaboration
AU - Pierre Auger Collaboration
AU - ALMA Collaboration
AU - Euro VLBI Team
AU - Pi of the Sky Collaboration
AU - Chandra Team at McGill University
AU - DFN: Desert Fireball Network
AU - ATLAS
AU - High Time Resolution Universe Survey
AU - RIMAS and RATIR
AU - SKA South Africa/MeerKAT
AU - Abbott, B. P.
AU - Abbott, R.
AU - Abbott, T. D.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
AU - Adams, T.
AU - Addesso, P.
AU - Adhikari, R. X.
AU - Adya, V. B.
AU - Affeldt, C.
AU - Afrough, M.
AU - Agarwal, B.
AU - Agathos, M.
AU - Agatsuma, K.
AU - Aggarwal, N.
AU - Aguiar, O. D.
AU - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
AU - Allen, B.
AU - Allen, G.
AU - Allocca, A.
AU - Altin, P. A.
AU - Amato, A.
AU - Ananyeva, A.
AU - Anderson, S. B.
AU - Anderson, W. G.
AU - Angelova, S. V.
AU - Antier, S.
AU - Appert, S.
AU - Arai, K.
AU - Araya, M. C.
AU - Areeda, J. S.
AU - Arnaud, N.
AU - Arun, K. G.
AU - Ascenzi, S.
AU - Ashton, G.
AU - Ast, M.
AU - Aston, S. M.
AU - Astone, P.
AU - Atallah, D. V.
AU - Aufmuth, P.
AU - Aulbert, C.
AU - AultONeal, K.
AU - Austin, C.
AU - Avila-Alvarez, A.
AU - Babak, S.
AU - Bacon, P.
AU - Bader, M. K.M.
AU - Bae, S.
AU - Baker, P. T.
AU - Baldaccini, F.
AU - Ballardin, G.
AU - Ballmer, S. W.
AU - Banagiri, S.
AU - Barayoga, J. C.
AU - Barclay, S. E.
AU - Barish, B. C.
AU - Barker, D.
AU - Barkett, K.
AU - Barone, F.
AU - Barr, B.
AU - Barsotti, L.
AU - Barsuglia, M.
AU - Barta, D.
AU - Barthelmy, S. D.
AU - Bartlett, J.
AU - Bartos, I.
AU - Bassiri, R.
AU - Basti, A.
AU - Batch, J. C.
AU - Bawaj, M.
AU - Bayley, J. C.
AU - Bazzan, M.
AU - Bécsy, B.
AU - Beer, C.
AU - Bejger, M.
AU - Belahcene, I.
AU - Bell, A. S.
AU - Berger, B. K.
AU - Bergmann, G.
AU - Bero, J. J.
AU - Berry, C. P.L.
AU - Bersanetti, D.
AU - Bertolini, A.
AU - Betzwieser, J.
AU - Bhagwat, S.
AU - Bhandare, R.
AU - Bilenko, I. A.
AU - Billingsley, G.
AU - Billman, C. R.
AU - Birch, J.
AU - Birney, R.
AU - Birnholtz, O.
AU - Biscans, S.
AU - Biscoveanu, S.
AU - Bisht, A.
AU - Bitossi, M.
AU - Keane, E. F.
N1 - Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.
PY - 2017/1/1
Y1 - 2017/1/1
N2 - 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 ~1.7 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 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☉. 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 ~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 ∼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.
AB - 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 ~1.7 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 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☉. 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 ~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 ∼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.
KW - Gravitational waves
KW - Stars: neutron
UR - https://www.scopus.com/pages/publications/85037171677
U2 - 10.3847/2041-8213/aa91c9
DO - 10.3847/2041-8213/aa91c9
M3 - Article
SN - 2041-8205
VL - 848
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 2
M1 - L12
ER -