Properties of the Binary Neutron Star Merger GW170817

被引：1043

作者：

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

Abbott, R. ^{[1
]}

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

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

Ackley, K. ^{[5
]}

Adams, C. ^{[6
]}

Adams, T. ^{[7
]}

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

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

Adya, V. B. ^{[10
,11
]}

Affeldt, C. ^{[10
,11
]}

Agarwal, B. ^{[12
]}

Agathos, M. ^{[13
]}

Agatsuma, K. ^{[14
]}

Aggarwal, N. ^{[15
]}

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

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

Ain, A. ^{[19
]}

Ajith, P. ^{[20
]}

Allen, B. ^{[10
,11
,21
]}

Allen, G. ^{[12
]}

Allocca, A. ^{[22
,23
]}

Aloy, M. A. ^{[24
]}

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

Amato, A. ^{[26
]}

Ananyeva, A. ^{[1
]}

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
]}

Arene, M. ^{[30
]}

Arnaud, N. ^{[28
,31
]}

Arun, K. G. ^{[32
]}

Ascenzi, S. ^{[33
,34
]}

Ashton, G. ^{[5
]}

Ast, M. ^{[35
]}

Aston, S. M. ^{[6
]}

Astone, P. ^{[36
]}

Atallah, D., V ^{[37
]}

Aubin, F. ^{[38
]}

Aufmuth, P. ^{[11
]}

Aulbert, C. ^{[10
]}

AultONeal, K. ^{[39
]}

Austin, C. ^{[2
]}

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

Babak, S. ^{[30
,40
]}

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 Angelo, INFN, Sez Napoli, I-80126 Naples, Italy

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

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

[7] Univ Savoie Mont Blanc, LAPP, Univ Grenoble Alpes, CNRS IN2P3, F-74941 Annecy, France

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

[9] INFN, Sez Napoli, I-80100 Naples, Italy

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

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

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

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

[14] Nikhef, Sci Pk 105, NL-1098 XG Amsterdam, Netherlands

[15] MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA

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

[17] GSSI, I-67100 Laquila, Italy

[18] INFN, 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, WI 53201 USA

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

[23] INFN, Sez Pisa, I-56127 Pisa, Italy

[24] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain

[25] Australian Natl Univ, 0zGrav, Canberra, ACT 0200, Australia

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

[27] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland

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

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

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

[31] EGO, I-56021 Pisa, Italy

[32] Chennai Math Inst, Madras 603103, Tamil Nadu, India

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

[34] INFN, Sez Roma Tor Vergata, I-00133 Rome, Italy

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

[36] INFN, Sez Roma, I-00185 Rome, Italy

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

[38] Univ Grenoble Alpes, Univ Savoie Mont Blanc, LAPP, CNRS IN2P3, F-74941 Annecy, France

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

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

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

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

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

[44] INFN, Sez Perugia, I-06123 Perugia, Italy

[45] Syracuse Univ, Syracuse, NY 13244 USA

[46] Univ Minnesota, Minneapolis, MN 55455 USA

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

[48] LIG0 Hanford Observ, Richland, WA 99352 USA

[49] Caltech CaRT, Pasadena, CA 91125 USA

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

来源：

PHYSICAL REVIEW X | 2019年 / 9卷 / 01期

基金：

澳大利亚研究理事会; 中国国家自然科学基金; 新加坡国家研究基金会; 俄罗斯基础研究基金会; 俄罗斯科学基金会; 瑞士国家科学基金会; 匈牙利科学研究基金会;

关键词：

INSPIRALING COMPACT BINARIES; GAMMA-RAY BURSTS; GRAVITATIONAL-WAVES; ELECTROMAGNETIC COUNTERPART; PARAMETER-ESTIMATION; LIGHT CURVES; KILONOVA; RADIATION; EQUATION; MATTER;

D O I：

10.1103/PhysRevX.9.011001

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

On August 17, 2017, the Advanced LIGO and Advanced Virgo gravitational-wave detectors observed a low-mass compact binary inspiral. The initial sky localization of the source of the gravitational-wave signal, GW170817, allowed electromagnetic observatories to identify NGC 4993 as the host galaxy. In this work, we improve initial estimates of the binary's properties, including component masses, spins, and tidal parameters, using the known source location, improved modeling, and recalibrated Virgo data. We extend the range of gravitational-wave frequencies considered down to 23 Hz, compared to 30 Hz in the initial analysis. We also compare results inferred using several signal models, which are more accurate and incorporate additional physical effects as compared to the initial analysis. We improve the localization of the gravitational-wave source to a 90% credible region of 16 deg(2). We find tighter constraints on the masses, spins, and tidal parameters, and continue to find no evidence for nonzero component spins. The component masses are inferred to lie between 1.00 and 1.89 M-circle dot when allowing for large component spins, and to lie between 1.16 and 1.60 M-circle dot (with a total mass 2.73(-0.01)(+0.04) M-circle dot) when the spins are restricted to be within the range observed in Galactic binary neutron stars. Using a precessing model and allowing for large component spins, we constrain the dimensionless spins of the components to be less than 0.50 for the primary and 0.61 for the secondary. Under minimal assumptions about the nature of the compact objects, our constraints for the tidal deformability parameter (Lambda) over tilde are (0,630) when we allow for large component spins, and 300(-230)(+420) (using a 90% highest posterior density interval) when restricting the magnitude of the component spins, ruling out several equation-of-state models at the 90% credible level. Finally, with LIGO and GEO600 data, we use a Bayesian analysis to place upper limits on the amplitude and spectral energy density of a possible postmerger signal.

引用

页数：32

共 167 条

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