Статья

INTEGRAL Detection of the First Prompt Gamma-Ray Signal Coincident with the Gravitational-wave Event GW170817

V. SavchenkoISDC, Department of Astronomy, University of Geneva, Chemin d’Écogia, 16 CH-1290 Versoix, SwitzerlandC. FerrignoISDC, Department of Astronomy, University of Geneva, Chemin d’Écogia, 16 CH-1290 Versoix, SwitzerlandE. KuulkersEuropean Space Research and Technology Centre (ESA/ESTEC), Keplerlaan 1, 2201 AZ Noordwijk, The NetherlandsA. BazzanoINAF-Institute for Space Astrophysics and Planetology, Via Fosso del Cavaliere 100, I-00133-Rome, ItalyE. BozzoISDC, Department of Astronomy, University of Geneva, Chemin d’Écogia, 16 CH-1290 Versoix, SwitzerlandS. BrandtDTU Space, National Space Institute Elektrovej, Building 327 DK-2800 Kongens Lyngby, DenmarkJ. ChenevezDTU Space, National Space Institute Elektrovej, Building 327 DK-2800 Kongens Lyngby, DenmarkT. J.-L. CourvoisierISDC, Department of Astronomy, University of Geneva, Chemin d’Écogia, 16 CH-1290 Versoix, SwitzerlandR. DiehlMax-Planck-Institut für Extraterrestrische Physik, Garching, GermanyA. DomingoCentro de Astrobiología (CAB-CSIC/INTA, ESAC Campus), Camino bajo del Castillo S/N, E-28692 Villanueva de la Cañada, Madrid, SpainL. HanlonSpace Science Group, School of Physics, University College Dublin, Belfield, Dublin 4, IrelandE. JourdainIRAP, Université de Toulouse, CNRS, UPS, CNES; 9 Av. Roche, F-31028 Toulouse, FranceA. von KienlinMax-Planck-Institut für Extraterrestrische Physik, Garching, GermanyP. LaurentAPC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris Sorbonne Paris Cité, 10 rue Alice Domont et Léonie Duquet, F-75205 Paris Cedex 13, FranceF. LebrunAPC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris Sorbonne Paris Cité, 10 rue Alice Domont et Léonie Duquet, F-75205 Paris Cedex 13, FranceA. LutovinovMoscow Institute of Physics and Technology, Institutskiy per. 9, 141700 Dolgoprudny, Moscow Region, RussiaA. Martin-CarrilloSpace Science Group, School of Physics, University College Dublin, Belfield, Dublin 4, IrelandS. MereghettiINAF, IASF-Milano, via E.Bassini 15, I-20133 Milano, ItalyL. NatalucciINAF-Institute for Space Astrophysics and Planetology, Via Fosso del Cavaliere 100, I-00133-Rome, ItalyJ. RodiINAF-Institute for Space Astrophysics and Planetology, Via Fosso del Cavaliere 100, I-00133-Rome, ItalyJ.-P. RoquesIRAP, Université de Toulouse, CNRS, UPS, CNES; 9 Av. Roche, F-31028 Toulouse, FranceR. SunyaevMax Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, D-85741 Garching b. München, GermanyP. UbertiniINAF-Institute for Space Astrophysics and Planetology, Via Fosso del Cavaliere 100, I-00133-Rome, Italy

2017en

ABI

Аннотация

Abstract We report the INTernational Gamma-ray Astrophysics Laboratory ( INTEGRAL ) detection of the short gamma-ray burst GRB 170817A (discovered by Fermi -GBM) with a signal-to-noise ratio of 4.6, and, for the first time, its association with the gravitational waves (GWs) from binary neutron star (BNS) merging event GW170817 detected by the LIGO and Virgo observatories. The significance of association between the gamma-ray burst observed by INTEGRAL and GW170817 is 3.2σ, while the association between the Fermi -GBM and INTEGRAL detections is 4.2σ. GRB 170817A was detected by the SPI-ACS instrument about 2 s after the end of the GW event. We measure a fluence of (1.4 ± 0.4 ± 0.6) × 10 −7 erg cm −2 (75–2000 keV), where, respectively, the statistical error is given at the 1σ confidence level, and the systematic error corresponds to the uncertainty in the spectral model and instrument response. We also report on the pointed follow-up observations carried out by INTEGRAL , starting 19.5 hr after the event, and lasting for 5.4 days. We provide a stringent upper limit on any electromagnetic signal in a very broad energy range, from 3 keV to 8 MeV, constraining the soft gamma-ray afterglow flux to <7.1 × 10 −11 erg cm −2 s −1 (80–300 keV). Exploiting the unique capabilities of INTEGRAL , we constrained the gamma-ray line emission from radioactive decays that are expected to be the principal source of the energy behind a kilonova event following a BNS coalescence. Finally, we put a stringent upper limit on any delayed bursting activity, for example, from a newly formed magnetar.

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Идентификаторы

DOI: 10.3847/2041-8213/aa8f94

Цитирования и источники

Цитирований: 6Использованных источников: 0

Показатели — AkademScholar