Multi-messenger Observations of a Binary Neutron Star Merger

doi:10.3847/2041-8213/aa91c9

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	Multi-messenger Observations of a Binary Neutron Star Merger
	The Insight-HXMT Collaboration
刊名	ASTROPHYSICAL JOURNAL LETTERS
	2017
卷号	848 期号:2 页码:L12
关键词	gravitational waves stars: neutron
ISSN号	2041-8205
DOI	10.3847/2041-8213/aa91c9
文献子类	Article
英文摘要	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 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.
电子版国际标准刊号	2041-8213
WOS关键词	GAMMA-RAY BURSTS ; NEARBY SUPERNOVA RATES ; GRAVITATIONAL-WAVES ; RELATIVISTIC GRAVITY ; PULSAR PSR-1913+16 ; OPTICAL AFTERGLOWS ; COMPACT OBJECTS ; RADIO TELESCOPE ; CLOSE BINARIES ; BLACK-HOLES
WOS研究方向	Astronomy & Astrophysics
语种	英语
WOS记录号	WOS:000413211000001
内容类型	期刊论文
源URL	[http://ir.ihep.ac.cn/handle/311005/284674]
专题	高能物理研究所_粒子天体物理中心
作者单位	中国科学院高能物理研究所
推荐引用方式 GB/T 7714	The Insight-HXMT Collaboration. Multi-messenger Observations of a Binary Neutron Star Merger[J]. ASTROPHYSICAL JOURNAL LETTERS,2017,848(2):L12.
APA	The Insight-HXMT Collaboration.(2017).Multi-messenger Observations of a Binary Neutron Star Merger.ASTROPHYSICAL JOURNAL LETTERS,848(2),L12.
MLA	The Insight-HXMT Collaboration."Multi-messenger Observations of a Binary Neutron Star Merger".ASTROPHYSICAL JOURNAL LETTERS 848.2(2017):L12.