Multi-messenger Observations of a Binary Neutron Star Merger

被引：2710

作者：

Abbott, B. P. ^{[1
]}

Abbott, R. ^{[1
]}

Abbott, T. D. ^{[2
]}

Acernese, F. ^{[3
,4
]}

Ackley, K. ^{[5
,6
,543
]}

Adams, C. ^{[7
]}

Adams, T.

Addesso, P. ^{[8
,9
]}

Adhikari, R. X. ^{[1
]}

Adya, V. B. ^{[10
]}

Affeldt, C. ^{[10
]}

Afrough, M. ^{[11
]}

Agarwal, B. ^{[12
]}

Agathos, M. ^{[13
]}

Agatsuma, K. ^{[14
,114
]}

Aggarwal, N. ^{[15
,115
]}

Aguiar, O. D. ^{[16
]}

Aiello, L. ^{[17
,18
]}

Ain, A. ^{[19
]}

Ajith, P. ^{[20
]}

Allen, B. ^{[10
,21
,22
]}

Allen, G. ^{[12
]}

Allocca, A. ^{[23
,24
]}

Altin, P. A. ^{[25
]}

Amato, A. ^{[26
]}

Ananyeva, A. ^{[1
,11
]}

Anderson, S. B. ^{[1
]}

Anderson, W. G. ^{[21
]}

Angelova, S. V. ^{[27
]}

Antier, S. ^{[28
]}

Appert, S. ^{[1
]}

Arai, K. ^{[1
]}

Araya, M. C. ^{[1
]}

Areeda, J. S. ^{[29
]}

Arnaud, N. ^{[28
,30
]}

Arun, K. G. ^{[31
]}

Ascenzi, S. ^{[32
,33
]}

Ashton, G. ^{[10
]}

Ast, M. ^{[34
]}

Aston, S. M.

Astone, P. ^{[35
]}

Atallah, D. V. ^{[36
]}

Aufmuth, P. ^{[22
]}

Aulbert, C. ^{[10
]}

AultONeal, K. ^{[37
]}

Austin, C. ^{[2
]}

Avila-Alvarez, A. ^{[29
]}

Babak, S. ^{[38
]}

Bacon, P. ^{[39
]}

Bader, M. K. M. ^{[14
,114
]}

机构：

[1] CALTECH, LIGO, Pasadena, CA 91125 USA

[2] Louisiana State Univ, Baton Rouge, LA 70803 USA

[3] Univ Salerno, I-84084 Salerno, Italy

[4] Complesso Univ Monte S Angelo04, Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy

[5] Univ Florida, Gainesville, FL 32611 USA

[6] Monash Univ, Sch Phys & Astron, OzGrav, Clayton, Vic 3800, Australia

[7] LIGO Livingston Observ, Livingston, LA 70754 USA

[8] Univ Sannio Benevento, I-82100 Benevento, Italy

[9] Ist Nazl Fis Nucl, Sez Napoli, I-80100 Naples, Italy

[10] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany

[11] Univ Mississippi, University, MS 38677 USA

[12] Univ Illinois, NCSA, Urbana, IL 61801 USA

[13] Univ Cambridge, Cambridge CB2 1TN, England

[14] Nikhef, Sci Pk, NL-1098 XG Amsterdam, Netherlands

[15] MIT, LIGO, Cambridge, MA 02139 USA

[16] Inst Nacl Pesquisas Espaciais, Sao Jose Campos, BR-12227010 Sao Paulo, Brazil

[17] GSSI, I-67100 Laquila, Italy

[18] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67100 Assergi, Italy

[19] Inter Univ, Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[20] Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bengaluru 560089, India

[21] Univ Wisconsin Milwaukee, Milwaukee, WI 53201 USA

[22] Leibniz Univ Hannover, D-30167 Hannover, Germany

[23] Univ Pisa, I-56127 Pisa, Italy

[24] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[25] Australian Natl Univ, OzGrav, Canberra, ACT 0200, Australia

[26] CNRS, IN2P3, LMA, F-69622 Villeurbanne, France

[27] Univ Weast Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland

[28] Univ Paris Saclay, Univ Paris Sud, CNRS, IN2P3,LAL, F-91898 Orsay, France

[29] Calif State Univ Fullerton, Fullerton, CA 92831 USA

[30] EGO, I-56021 Pisa, Italy

[31] Chennai Math Inst, Chennai 603103, Tamil Nadu, India

[32] Univ Roma Tor Vergata, I-00133 Rome, Italy

[33] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

[34] Univ Hamburg, D-22761 Hamburg, Germany

[35] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy

[36] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales

[37] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA

[38] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany

[39] Univ Paris Diderot, CNRS, IN2P3,Sorbonne Paris Cite, APC,AstroParticule & Cosmol,CEA Irfu,Observ Paris, F-75205 Paris 13, France

[40] Korea Inst Sci & Technol Informat, Daejeon 34141, South Korea

[41] West Virginia Univ, Morgantown, WV 26506 USA

[42] Univ Perugia, I-06123 Perugia, Italy

[43] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[44] Syracuse Univ, Syracuse, NY 13244 USA

[45] Univ Minnesota, Minneapolis, MN 55455 USA

[46] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland

[47] LIGO Hanford Observ, Richland, WA 99352 USA

[48] Caltech CaRT, Pasadena, CA 91125 USA

[49] RMKI, Wigner RCP, Konkoly Thege Miklos Ut 29-33, H-1121 Budapest, Hungary

[50] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2017年 / 848卷 / 02期

基金：

瑞典研究理事会; 日本学术振兴会; 美国国家科学基金会; 俄罗斯科学基金会; 新加坡国家研究基金会; 澳大利亚研究理事会; 以色列科学基金会; 瑞士国家科学基金会; 欧盟地平线“2020”; 加拿大自然科学与工程研究理事会; 巴西圣保罗研究基金会; 中国国家自然科学基金; 奥地利科学基金会; 英国科学技术设施理事会; 俄罗斯基础研究基金会; 欧洲研究理事会; 匈牙利科学研究基金会; 爱尔兰科学基金会;

关键词：

gravitational waves; stars: neutron; GAMMA-RAY BURST; NEARBY SUPERNOVA RATES; GRAVITATIONAL-WAVES; HOST GALAXY; AFTERGLOW; PULSAR; EVOLUTION; REDSHIFT; IMAGER; NUCLEOSYNTHESIS;

D O I：

10.3847/2041-8213/aa91c9

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

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.

引用

页数：59

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