Directly comparing GW150914 with numerical solutions of Einstein's equations for binary black hole coalescence

被引：118

作者：

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

Abbott, R. ^{[1
]}

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

Abernathy, M. R. ^{[3
]}

Acernese, F. ^{[4
,5
]}

Ackley, K. ^{[6
]}

Adams, C. ^{[7
]}

Adams, T. ^{[8
]}

Addesso, P. ^{[9
,10
]}

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

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

Affeldt, C. ^{[11
]}

Agathos, M. ^{[12
]}

Agatsuma, K. ^{[12
]}

Aggarwal, N. ^{[13
]}

Aguiar, O. D. ^{[14
]}

Aiello, L. ^{[15
,16
]}

Ain, A. ^{[17
]}

Ajith, P. ^{[18
]}

Allen, B. ^{[11
,19
,20
]}

Allocca, A. ^{[21
,22
]}

Altin, P. A. ^{[23
]}

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

Anderson, W. G. ^{[19
]}

Arai, K. ^{[1
]}

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

Arceneaux, C. C. ^{[24
]}

Areeda, J. S. ^{[25
]}

Arnaud, N. ^{[26
]}

Arun, K. G. ^{[27
]}

Ascenzi, S. ^{[16
,28
]}

Ashton, G. ^{[29
]}

Ast, M. ^{[30
]}

Aston, S. M. ^{[7
]}

Astone, P. ^{[31
]}

Aufmuth, P. ^{[20
]}

Aulbert, C. ^{[11
]}

Babak, S. ^{[32
]}

Bacon, P. ^{[33
]}

Bader, M. K. M. ^{[12
]}

Baker, P. T. ^{[34
]}

Baldaccini, F. ^{[35
,36
]}

Ballardin, G. ^{[37
]}

Ballmer, S. W. ^{[38
]}

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

Barclay, S. E. ^{[39
]}

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

Barker, D. ^{[40
]}

Barone, F. ^{[4
,5
]}

Barr, B. ^{[39
]}

机构：

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

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

[3] Amer Univ, Washington, DC 20016 USA

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

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

[6] Univ Florida, Gainesville, FL 32611 USA

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

[8] Univ Savoie Mont Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France

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

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

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

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

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

[14] Inst Nacl Pesquisas Espaciais, 12227-010 Sao Jose Campos, Sao Paulo, Brazil

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

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

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

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

[19] Univ Wisconsin, Milwaukee, WI 53201 USA

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

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

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

[23] Australian Natl Univ, Canberra, ACT 0200, Australia

[24] Univ Mississippi, University, MS 38677 USA

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

[26] Univ Paris 11, LAL, Univ Paris Saclay, CNRS,IN2P3, F-91405 Orsay, France

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

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

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

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

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

[32] Max Planck Inst Gravitat phys, Albert Einstein Inst, D-14476 Potsdam, Germany

[33] Univ Paris Diderot, APC, Observ Paris, CNRS,IN2P3,CEA,Irfu, Sorbonne Paris Cite, F-75205 Paris 13, France

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

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

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

[37] EGO, I-56021 Pisa, Italy

[38] Syracuse Univ, Syracuse, NY 13244 USA

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

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

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

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

[43] Stanford Univ, Stanford, CA 94305 USA

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

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

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

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

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

[49] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy

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

来源：

PHYSICAL REVIEW D | 2016年 / 94卷 / 06期

基金：

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; 新加坡国家研究基金会; 澳大利亚研究理事会;

关键词：

GRAVITATIONAL-WAVES; INITIAL DATA; EVOLUTION; RELATIVITY; MERGER; STARS;

D O I：

10.1103/PhysRevD.94.064035

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We compare GW150914 directly to simulations of coalescing binary black holes in full general relativity, including several performed specifically to reproduce this event. Our calculations go beyond existing semianalytic models, because for all simulations-including sources with two independent, precessing spins - we perform comparisons which account for all the spin-weighted quadrupolar modes, and separately which account for all the quadrupolar and octopolar modes. Consistent with the posterior distributions reported by Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016)] (at the 90% credible level), we find the data are compatible with a wide range of nonprecessing and precessing simulations. Follow-up simulations performed using previously estimated binary parameters most resemble the data, even when all quadrupolar and octopolar modes are included. Comparisons including only the quadrupolar modes constrain the total redshifted mass M-z epsilon [64 M-circle dot - 82 M-circle dot], mass ratio 1/q = m(2)/m(1) epsilon [0.6; 1], and effective aligned spin chi(eff) epsilon [-0.3, 0.2] where chi(eff) = (S-1/m(1)+S-2/m(2)). (L) over cap /M. Including both quadrupolar and octopolar modes, we find the mass ratio is even more tightly constrained. Even accounting for precession, simulations with extreme mass ratios and effective spins are highly inconsistent with the data, at any mass. Several nonprecessing and precessing simulations with similar mass ratio and chi(eff) are consistent with the data. Though correlated, the components' spins (both in magnitude and directions) are not significantly constrained by the data: the data is consistent with simulations with component spin magnitudes a(1,2) up to at least 0.8, with random orientations. Further detailed follow-up calculations are needed to determine if the data contain a weak imprint from transverse (precessing) spins. For nonprecessing binaries, interpolating between simulations, we reconstruct a posterior distribution consistent with previous results. The final black hole's redshifted mass is consistent with M-f,M-z in the range 64.0 M-circle dot - 73.5 M-circle dot and the final black hole's dimensionless spin parameter is consistent with a(f) = 0.62-0.73. As our approach invokes no intermediate approximations to general relativity and can strongly reject binaries whose radiation is inconsistent with the data, our analysis provides a valuable complement to Abbott et al.

引用

页数：30

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