Effects of waveform model systematics on the interpretation of GW150914

被引：127

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
,146
]}

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

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

Affeldt, C. ^{[10
]}

Agathos, M. ^{[11
]}

Agatsuma, K. ^{[11
]}

Aggarwal, N. ^{[12
]}

Aguiar, O. D.

Aiello, L. ^{[14
,15
]}

Ain, A. ^{[13
,16
,105
]}

Ajith, P. ^{[17
]}

Allen, B. ^{[10
,18
,19
]}

Allocca, A. ^{[20
,21
]}

Altin, P. A. ^{[22
]}

Ananyeva, A. ^{[1
]}

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

Anderson, W. G. ^{[18
]}

Appert, S. ^{[1
]}

Arai, K. ^{[1
]}

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

Areeda, J. S. ^{[23
]}

Arnaud, N. ^{[24
]}

Arun, K. G. ^{[25
]}

Ascenzi, S. ^{[15
,26
]}

Ashton, G. ^{[10
]}

Ast, M. ^{[27
]}

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

Astone, P. ^{[28
]}

Aufmuth, P. ^{[19
]}

Aulbert, C. ^{[10
]}

Avila-Alvarez, A. ^{[23
]}

Babak, S. ^{[29
]}

Bacon, P. ^{[30
]}

Bader, M. K. M. ^{[11
]}

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

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

Ballardin, G. ^{[34
]}

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

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

Barclay, S. E. ^{[32
]}

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

Barker, D. ^{[37
]}

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, Fisciano, I-84084 Salerno, Italy

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

[6] Univ Florida, Gainesville, FL 32611 USA

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[34] 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] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland

[44] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA

[45] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA

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

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

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

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

[50] Lomonosov Moscow State Univ, Fac Phys, Moscow 119991, Russia

来源：

CLASSICAL AND QUANTUM GRAVITY | 2017年 / 34卷 / 10期

基金：

美国国家科学基金会; 巴西圣保罗研究基金会; 匈牙利科学研究基金会; 新加坡国家研究基金会; 俄罗斯基础研究基金会;

关键词：

gravitational waves; numerical relativity; parameter estimation; waveform models; systematic errors; GW150914; GRAVITATIONAL-WAVES; INITIAL DATA; RADIATION; BINARIES;

D O I：

10.1088/1361-6382/aa6854

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Parameter estimates of GW150914 were obtained using Bayesian inference, based on three semi-analytic waveform models for binary black hole coalescences. These waveform models differ from each other in their treatment of black hole spins, and all three models make some simplifying assumptions, notably to neglect sub-dominant waveform harmonic modes and orbital eccentricity. Furthermore, while the models are calibrated to agree with waveforms obtained by full numerical solutions of Einstein's equations, any such calibration is accurate only to some non-zero tolerance and is limited by the accuracy of the underlying phenomenology, availability, quality, and parameter-space coverage of numerical simulations. This paper complements the original analyses of GW150914 with an investigation of the effects of possible systematic errors in the waveform models on estimates of its source parameters. To test for systematic errors we repeat the original Bayesian analysis on mock signals from numerical simulations of a series of binary configurations with parameters similar to those found for GW150914. Overall, we find no evidence for a systematic bias relative to the statistical error of the original parameter recovery of GW150914 due to modeling approximations or modeling inaccuracies. However, parameter biases are found to occur for some configurations disfavored by the data of GW150914: for binaries inclined edge-on to the detector over a small range of choices of polarization angles, and also for eccentricities greater than similar to 0.05. For signals with higher signal-to-noise ratio than GW150914, or in other regions of the binary parameter space (lower masses, larger mass ratios, or higher spins), we expect that systematic errors in current waveform models may impact gravitational-wave measurements, making more accurate models desirable for future observations.

引用

页数：48

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