{"paper":{"title":"Multi-messenger Observations of a Binary Neutron Star Merger","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"AGILE Team, ALMA Collaboration, ANTARES Collaboration, ASKAP: Australian SKA Pathfinder, AST3, AstroSat Cadmium Zinc Telluride Imager Team, ATCA: Australia Telescope Compact Array, Atlas, CAASTRO Collaborations, Caltech- NRAO, DFN: Desert Fireball Network, DWF (Deeper, ePESSTO, Euro VLBI Team, Faster Program), Fermi GBM, GRAWITA: GRAvitational Wave Inaf TeAm, GROND, GROWTH, HAWC Collaboration, H.E.S.S. collaboration, High Time Resolution Universe Survey, IceCube Collaboration, IKI-GW Follow-up Collaboration, INTEGRAL, IPN Collaboration, JAGWAR, J-GEM, KU Collaboration, Las Cumbres Observatory Group, LIGO Scientific Collaboration, LOFAR Collaboration, LWA: Long Wavelength Array, MASTER Collaboration, MWA: Murchison Widefield Array, Nordic Optical Telescope, NuSTAR Collaborations, OzGrav, Pan-STARRS, Pi of the Sky Collaboration, RATIR, RIMAS, SALT Group, SKA South Africa/MeerKAT, Texas Tech University, The 1M2H Team, The BOOTES Collaboration, the CALET collaboration, The Chandra Team at McGill University, The Dark Energy Camera GW-EM Collaboration, The DES Collaboration, The DLT40 Collaboration, The Fermi Large Area Telescope Collaboration, The Insight-Hxmt Collaboration, the MAXI team, The Pierre Auger Collaboration, The Swift Collaboration, The VINROUGE Collaboration, TOROS: Transient Robotic Observatory of the South Collaboration, TTU-NRAO, TZAC Consortium, Virgo Collaboration, Wider","submitted_at":"2017-10-16T16:57:18Z","abstract_excerpt":"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 $\\sim$1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg$^2$ at a luminosity distance of $40^{+8}_{-8}$ Mpc and with component masses consistent with neutron stars. The component masses were la"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1710.05833","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}