English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/165029
Share/Impact:
Statistics
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL
Exportar a otros formatos:
Title

Multi-messenger Observations of a Binary Neutron Star

AuthorsLIGO Sci, Virgo, ANTARES and other Collaborations; Cano, Z.; Ugarte Postigo, Antonio de ; Thöne, Cristina Carina ; Hodosan, G.; Kann, D.A.; Izzo, L.; Castro-Tirado, Alberto J. ; Tello, J.C.; Hu, Y.D.; Zhang, B.B.; Cunniffe, R.; Agudo, Iván
KeywordsStars: neutron
Gravitational waves
Issue Date2017
CitationAstrophysical Journal Letters 848(2): L12 (2017)
AbstractOn 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 similar to 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 later measured to be in the range 0.86 to 2.26 M-circle dot. 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 similar to 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 similar to 10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position similar to 9 and similar to 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 NGC4993 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. © 2017. The American Astronomical Society. All rights reserved.
URIhttp://hdl.handle.net/10261/165029
Identifiersdoi: 10.3847/2041-8213/aa91c9
issn: 2041-8205
Appears in Collections:(IAA) Artículos
(CAB) Artículos
Files in This Item:
File Description SizeFormat 
IAA_2017_ApJL_848_L12.pdf3,19 MBAdobe PDFThumbnail
View/Open
Show full item record
 

Related articles:


WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.