Properties of the Binary Black Hole Merger GW150914

被引：968

作者：

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

Abbott, R. ^{[1
]}

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

Abernathy, M. R. ^{[1
]}

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

Ackley, K. ^{[5
]}

Adams, C. ^{[6
]}

Adams, T. ^{[7
]}

Addesso, P. ^{[3
]}

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

Adya, V. B. ^{[8
]}

Affeldt, C. ^{[8
]}

Agathos, M. ^{[9
]}

Agatsuma, K. ^{[9
]}

Aggarwal, N. ^{[10
]}

Aguiar, O. D. ^{[11
]}

Aiello, L. ^{[12
,13
]}

Ain, A. ^{[14
]}

Ajith, P. ^{[15
]}

Allen, B. ^{[8
,16
,17
]}

Allocca, A. ^{[18
,19
]}

Altin, P. A. ^{[20
]}

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

Anderson, W. G. ^{[16
]}

Arai, K. ^{[1
]}

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

Arceneaux, C. C. ^{[21
]}

Areeda, J. S. ^{[22
]}

Arnaud, N. ^{[23
]}

Arun, K. G. ^{[24
]}

Ascenzi, S. ^{[13
,25
]}

Ashton, G. ^{[26
]}

Ast, M. ^{[27
]}

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

Astone, P. ^{[28
]}

Aufmuth, P. ^{[8
]}

Aulbert, C. ^{[8
]}

Babak, S. ^{[29
]}

Bacon, P. ^{[30
]}

Bader, M. K. M. ^{[9
]}

Baker, P. T. ^{[31
]}

Baldaccini, F. ^{[32
,33
]}

Ballardin, G. ^{[34
]}

Ballmer, S. W. ^{[35
]}

Barayoga, J. C. ^{[1
]}

Barclay, S. E. ^{[36
]}

Barish, B. C. ^{[1
]}

Barker, D. ^{[37
]}

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

Barr, B. ^{[36
]}

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, Sez Napoli, Ist Nazl Fis Nucl, I-80126 Naples, Italy

[5] Univ Florida, Gainesville, FL 32611 USA

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

[7] Univ Savoie Mt Blanc, Lab Annecy Le Vieux Phys Particules LAPP, CNRS IN2P3, F-74941 Annecy Le Vieux, France

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

[9] NIKHEF H, Sci Pk, NL-1098 XG Amsterdam, Netherlands

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

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

[12] Gran Sasso Sci Inst, Ist Nazl Fis Nucl, I-67100 Laquila, Italy

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

[14] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[15] Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bangalore 560012, Karnataka, India

[16] Univ Wisconsin, Milwaukee, WI 53201 USA

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

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

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

[20] Australian Natl Univ, GPO Box 4, Canberra, ACT 0200, Australia

[21] Univ Mississippi, University, MS 38677 USA

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

[23] Univ Paris Saclay, Univ Paris 11, LAL, CNRS IN2P3, F-91400 Orsay, France

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

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

[26] Univ Southampton, Southampton SO17 1BJ, Hants, England

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

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

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

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

[31] Montana State Univ, Bozeman, MT 59717 USA

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

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

[34] European Gravitat Observ EGO, I-56021 Pisa, Italy

[35] Syracuse Univ, Syracuse, NY 13244 USA

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

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

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

[39] Columbia Univ, New York, NY 10027 USA

[40] Stanford Univ, Stanford, CA 94305 USA

[41] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy

[42] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[43] CAMK PAN, PL-00716 Warsaw, Poland

[44] Univ Birmingham, Birmingham B15 2TT, W Midlands, England

[45] Univ Genoa, I-16146 Genoa, Italy

[46] Ist Nazl Fis Nucl, Sez Genova, Via Dodecaneso 33, I-16146 Genoa, Italy

[47] RRCAT, Indore 452013, Madhya Pradesh, India

[48] Moscow MV Lomonosov State Univ, Fac Phys, Moscow 119991, Russia

[49] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland

[50] Univ Western Australia, Crawley, WA 6009, Australia

来源：

PHYSICAL REVIEW LETTERS | 2016年 / 116卷 / 24期

基金：

新加坡国家研究基金会; 俄罗斯基础研究基金会; 美国国家科学基金会; 英国科学技术设施理事会; 匈牙利科学研究基金会; 俄罗斯科学基金会; 澳大利亚研究理事会;

关键词：

INSPIRALING COMPACT BINARIES; GRAVITATIONAL WAVE-FORMS; PARAMETER-ESTIMATION; ADVANCED LIGO; MAXIMUM MASS; RADIATION; X-1; STELLAR; SIGNALS; OBJECT;

D O I：

10.1103/PhysRevLett.116.241102

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

On September 14, 2015, the Laser Interferometer Gravitational-Wave Observatory (LIGO) detected a gravitational-wave transient (GW150914); we characterize the properties of the source and its parameters. The data around the time of the event were analyzed coherently across the LIGO network using a suite of accurate waveform models that describe gravitational waves from a compact binary system in general relativity. GW150914 was produced by a nearly equal mass binary black hole of masses 36(-4)(+5) M-circle dot and 29(-4)(-4) M-circle dot; for each parameter we report the median value and the range of the 90% credible interval. The dimensionless spin magnitude of the more massive black hole is bound to be < 0.7 ( at 90% probability). The luminosity distance to the source is 410(-180)(+160) Mpc, corresponding to a redshift 0.09(-0.04)(+0.03) assuming standard cosmology. The source location is constrained to an annulus section of 610 deg(2), primarily in the southern hemisphere. The binary merges into a black hole of mass 62(-4)(+4) M-circle dot and spin 0.67(-0.07)(+0.05). This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.

引用

页数：19

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