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A kilonova as the electromagnetic counterpart to a gravitational-wave source

Walton NA; Kankare E; Hamanowicz A; Prentice SJ; Terreran G; Heinze A; Pastorello A; Muller A; Kerzendorf WE; Sullivan M; Vos J; Martin-Carrillo A; Young DR; Maguire K; Angus CR; Klose S; Stubbs CW; Flors A; Chen TW; Willman M; Galbany L; Kostrzewa-Rutkowska Z; Cannizzaro G; Magee M; Rau A; Bulla M; Leloudas G; Szegedi H; Frohmaier C; Kowalski M; Homan DS; Gromadzki M; Cikota A; Manulis I; McBrien O; Pumo ML; Razza A; Harmanen J; Nordin J; Huber ME; Magnier EA; Rest A; Salmon L; Smith KW; Hook IM; Jerkstrand A; Kuncarayakti H; Sollerman J; Lawrence A; Waters C; Patat F; Rybicki KA; Hernandez MS; Inserra C; Smartt SJ; Palmerio JT; Taubenberger S; Cartier R; Dennefeld M; Hanlon L; Anderson JP; Onori F; Sim SA; Hodgkin ST; Ruiter AJ; Kotak R; Chambers KC; Barbarino C; Podsiadlowski P; Schweyer T; Pignata G; Wiseman P; Dessart L; Denneau L; Mattila S; Weiland H; De Cia A; Franckowiak A; Smith M; Yaron O; Wright DE; Gutierrez CP; Tonry J; Kromer M; Gonzalez-Gaitan S; Bulger J; Izzo L; Agliozzo C; Gal-Yam A; Taddia F; Dimitriadis G; Guelbenzu AN; Della Valle M; Seitenzahl IR; van Soelen B; Wainscoat RJ; Fraser M; Firth RE; Ashall C; Botticella MT; O'Neill D; Bauer FE; Lyman JD; Schady P; Clark P; Greiner J; Lowe TB; Elias-Rosa N; Cano Z; Jonker PG; Kruhler T; Berton M; Shingles LJ; Reynolds T; Wyrzykowski L; Heintz KE; Roy R; Stalder B; James PA; Coughlin M; Schultz ASB; Flewelling H

A kilonova as the electromagnetic counterpart to a gravitational-wave source

Walton NA
Kankare E
Hamanowicz A
Prentice SJ
Terreran G
Heinze A
Pastorello A
Muller A
Kerzendorf WE
Sullivan M
Vos J
Martin-Carrillo A
Young DR
Maguire K
Angus CR
Klose S
Stubbs CW
Flors A
Chen TW
Willman M
Galbany L
Kostrzewa-Rutkowska Z
Cannizzaro G
Magee M
Rau A
Bulla M
Leloudas G
Szegedi H
Frohmaier C
Kowalski M
Homan DS
Gromadzki M
Cikota A
Manulis I
McBrien O
Pumo ML
Razza A
Harmanen J
Nordin J
Huber ME
Magnier EA
Rest A
Salmon L
Smith KW
Hook IM
Jerkstrand A
Kuncarayakti H
Sollerman J
Lawrence A
Waters C
Patat F
Rybicki KA
Hernandez MS
Inserra C
Smartt SJ
Palmerio JT
Taubenberger S
Cartier R
Dennefeld M
Hanlon L
Anderson JP
Onori F
Sim SA
Hodgkin ST
Ruiter AJ
Kotak R
Chambers KC
Barbarino C
Podsiadlowski P
Schweyer T
Pignata G
Wiseman P
Dessart L
Denneau L
Mattila S
Weiland H
De Cia A
Franckowiak A
Smith M
Yaron O
Wright DE
Gutierrez CP
Tonry J
Kromer M
Gonzalez-Gaitan S
Bulger J
Izzo L
Agliozzo C
Gal-Yam A
Taddia F
Dimitriadis G
Guelbenzu AN
Della Valle M
Seitenzahl IR
van Soelen B
Wainscoat RJ
Fraser M
Firth RE
Ashall C
Botticella MT
O'Neill D
Bauer FE
Lyman JD
Schady P
Clark P
Greiner J
Lowe TB
Elias-Rosa N
Cano Z
Jonker PG
Kruhler T
Berton M
Shingles LJ
Reynolds T
Wyrzykowski L
Heintz KE
Roy R
Stalder B
James PA
Coughlin M
Schultz ASB
Flewelling H
Katso/Avaa
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NATURE PUBLISHING GROUP
doi:10.1038/nature24303
URI
http://www.nature.com/articles/nature24303
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Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2021042717450
Tiivistelmä
Gravitational waves were discovered with the detection of binary black-hole mergers(1) and they should also be detectable from lower-mass neutron-star mergers. These are predicted to eject material rich in heavy radioactive isotopes that can power an electromagnetic signal. This signal is luminous at optical and infrared wavelengths and is called a kilonova(2-5). The gravitational-wave source GW170817 arose from a binary neutron-star merger in the nearby Universe with a relatively well confined sky position and distance estimate(6). Here we report observations and physical modelling of a rapidly fading electromagnetic transient in the galaxy NGC 4993, which is spatially coincident with GW170817 and with a weak, short.-ray burst(7,8). The transient has physical parameters that broadly match the theoretical predictions of blue kilonovae from neutron-star mergers. The emitted electromagnetic radiation can be explained with an ejected mass of 0.04 +/- 0.01 solar masses, with an opacity of less than 0.5 square centimetres per gram, at a velocity of 0.2 +/- 0.1 times light speed. The power source is constrained to have a power-law slope of -1.2 +/- 0.3, consistent with radioactive powering from r-process nuclides. (The r-process is a series of neutron capture reactions that synthesise many of the elements heavier than iron.) We identify line features in the spectra that are consistent with light r-process elements (atomic masses of 90-140). As it fades, the transient rapidly becomes red, and a higher-opacity, lanthanide-rich ejecta component may contribute to the emission. This indicates that neutron-star mergers produce gravitational waves and radioactively powered kilonovae, and are a nucleosynthetic source of the r-process elements.
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