dc.identifier.uri |
http://www.repo.uni-hannover.de/handle/123456789/2609 |
|
dc.identifier.uri |
https://doi.org/10.15488/2583 |
|
dc.contributor.author |
Abbott, B.P.
|
|
dc.contributor.author |
et al.
|
|
dc.contributor.author |
LIGO Scientific Collaboration
|
|
dc.contributor.author |
Virgo Collaboration
|
|
dc.date.accessioned |
2018-01-18T09:13:07Z |
|
dc.date.available |
2018-01-18T09:13:07Z |
|
dc.date.issued |
2017 |
|
dc.identifier.citation |
Abbott, B.P. et al.: Multi-messenger observations of a binary neutron star merger. In: Astrophysical Journal Letters 848 (2017), Nr. 2, L12. DOI: https://doi.org/10.3847/2041-8213/aa91c9 |
|
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 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 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 . 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 ) 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 and 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 |
Bristol : Institute of Physics Publishing |
|
dc.relation.ispartofseries |
Astrophysical Journal Letters 848 (2017), Nr. 2 |
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dc.rights |
CC BY 3.0 Unported |
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dc.rights.uri |
https://creativecommons.org/licenses/by/3.0/ |
|
dc.subject |
binaries |
eng |
dc.subject |
Gravitationswelle |
ger |
dc.subject |
gravitational waves |
eng |
dc.subject |
stars: kinematics and dynamics |
eng |
dc.subject |
stars: neutron |
eng |
dc.subject.ddc |
530 | Physik
|
ger |
dc.title |
Multi-messenger observations of a binary neutron star merger |
|
dc.type |
Article |
|
dc.type |
Text |
|
dc.relation.doi |
https://doi.org/10.3847/2041-8213/aa91c9 |
|
dc.bibliographicCitation.issue |
2 |
|
dc.bibliographicCitation.volume |
848 |
|
dc.bibliographicCitation.firstPage |
L12 |
|
dc.description.version |
publishedVersion |
|
tib.accessRights |
frei zug�nglich |
|