The NINJA-2 project: detecting and characterizing gravitational waveforms modelled using numerical binary black hole simulations

被引：52

作者：

Aasi, J. ^{[1
]}

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

Abbott, R. ^{[1
]}

Abbott, T. ^{[2
]}

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

Accadia, T. ^{[3
]}

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

Ackley, K. ^{[6
]}

Adams, C. ^{[7
]}

Adams, T. ^{[8
]}

Addesso, P. ^{[5
]}

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

Affeldt, C. ^{[9
]}

Agathos, M. ^{[10
]}

Aggarwal, N. ^{[11
]}

Aguiar, O. D. ^{[12
]}

Ain, A. ^{[13
]}

Ajith, P. ^{[14
]}

Alemic, A. ^{[15
]}

Allen, B. ^{[9
,16
,17
]}

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

Amariutei, D. ^{[6
]}

Andersen, M. ^{[20
]}

Anderson, R. ^{[1
]}

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

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

Arai, K. ^{[1
]}

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

Arceneaux, C. ^{[21
]}

Areeda, J. ^{[22
]}

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

Astone, P. ^{[23
]}

Aufmuth, P. ^{[17
]}

Aulbert, C. ^{[9
]}

Austin, L. ^{[1
]}

Aylott, B. E. ^{[24
]}

Babak, S. ^{[25
]}

Baker, P. T. ^{[26
]}

Ballardin, G. ^{[27
]}

Ballmer, S. W. ^{[15
]}

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

Barbet, M. ^{[6
]}

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

Barker, D. ^{[28
]}

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

Barr, B. ^{[29
]}

Barsotti, L. ^{[11
]}

Barsuglia, M. ^{[30
]}

Barton, M. A. ^{[28
]}

Bartos, I. ^{[31
]}

机构：

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

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

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

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

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

[6] Univ Florida, Gainesville, FL 32611 USA

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

[8] Cardiff Univ, Cardiff CF24 3AA, Wales

[9] Albert Einstein Inst, Max Planck Inst Gravitationsphys, D-30167 Hannover, Germany

[10] Nikhef, NL-1098 XG Amsterdam, Netherlands

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

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

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

[14] Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India

[15] Syracuse Univ, Syracuse, NY 13244 USA

[16] Univ Wisconsin, Milwaukee, WI 53201 USA

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

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

[19] Univ Siena, I-53100 Siena, Italy

[20] Stanford Univ, Stanford, CA 94305 USA

[21] Univ Mississippi, University, MS 38677 USA

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

[23] Ist Nazl Fis Nucl, Sezi Roma, I-00185 Rome, Italy

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

[25] Albert Einstein Inst, Max Planck Inst Gravitationsphys, D-14476 Golm, Germany

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

[27] European Gravitat Observ, I-56021 Pisa, Italy

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

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

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

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

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

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

[34] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland

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

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

[37] San Jose State Univ, San Jose, CA 95192 USA

[38] Moscow MV Lomonosov State Univ, Fac Phys, Moscow 119992, Russia

[39] Univ Paris 11, CNRS, IN2P3, LAL, F-91898 Orsay, France

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

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

[42] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands

[43] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France

[44] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France

[45] Univ Lyon, CNRS, IN2P3, Lab Mat Avances, F-69622 Lyon, France

[46] Washington State Univ, Pullman, WA 99164 USA

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

[48] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Florence, Italy

[49] Univ Urbinon Carlo Bo, I-61029 Urbino, Italy

[50] Univ Oregon, Eugene, OR 97403 USA

来源：

CLASSICAL AND QUANTUM GRAVITY | 2014年 / 31卷 / 11期

基金：

英国科学技术设施理事会; 美国国家航空航天局; 新加坡国家研究基金会; 美国国家科学基金会; 奥地利科学基金会; 加拿大创新基金会; 澳大利亚研究理事会; 加拿大自然科学与工程研究理事会;

关键词：

numerical relativity; gravitational-wave astronomy; binary black; holes; NINJA; LIGO; Virgo; GAMMA-RAY BURSTS; COMPACT BINARIES; MASS-DISTRIBUTION; RADIATION; COSMOLOGY; EVOLUTION; MERGERS; SEARCH;

D O I：

10.1088/0264-9381/31/11/115004

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Numerical INJection Analysis (NINJA) project is a collaborative effort between members of the numerical relativity and gravitational-wave (GW) astrophysics communities. The purpose of NINJA is to study the ability to detect GWs emitted from merging binary black holes (BBH) and recover their parameters with next-generation GW observatories. We report here on the results of the second NINJA project, NINJA-2, which employs 60 complete BBH hybrid waveforms consisting of a numerical portion modelling the late inspiral, merger, and ringdown stitched to a post-Newtonian portion modelling the early inspiral. In a 'blind injection challenge' similar to that conducted in recent Laser Interferometer Gravitational Wave Observatory (LIGO) and Virgo science runs, we added seven hybrid waveforms to two months of data recoloured to predictions of Advanced LIGO (aLIGO) and Advanced Virgo (AdV) sensitivity curves during their first observing runs. The resulting data was analysed by GW detection algorithms and 6 of the waveforms were recovered with false alarm rates smaller than 1 in a thousand years. Parameter-estimation algorithms were run on each of these waveforms to explore the ability to constrain the masses, component angular momenta and sky position of these waveforms. We find that the strong degeneracy between the mass ratio and the BHs' angular momenta will make it difficult to precisely estimate these parameters with aLIGO and AdV. We also perform a large-scale Monte Carlo study to assess the ability to recover each of the 60 hybrid waveforms with early aLIGO and AdV sensitivity curves. Our results predict that early aLIGO and AdV will have a volume-weighted average sensitive distance of 300 Mpc (1 Gpc) for 10M circle dot + 10M circle dot (50M circle dot + 50M circle dot) BBH coalescences. We demonstrate that neglecting the component angular momenta in the waveform models used in matched-filtering will result in a reduction in sensitivity for systems with large component angular momenta. This reduction is estimated to be up to similar to 15% for 50M circle dot + 50M circle dot BBH coalescences with almost maximal angular momenta aligned with the orbit when using early aLIGO and AdV sensitivity curves.

引用

页数：45

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