Inspiral-merger-ringdown multipolar waveforms of nonspinning black-hole binaries using the effective-one-body formalism

被引：206

作者：

Pan, Yi ^{[1
,2
]}

Buonanno, Alessandra ^{[1
,2
]}

Boyle, Michael ^{[3
]}

Buchman, Luisa T. ^{[4
]}

Kidder, Lawrence E. ^{[3
]}

Pfeiffer, Harald P. ^{[5
]}

Scheel, Mark A. ^{[4
]}

机构：

[1] Univ Maryland, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA

[2] Univ Maryland, Joint Space Sci Inst, Dept Phys, College Pk, MD 20742 USA

[3] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA

[4] CALTECH, Pasadena, CA 91125 USA

[5] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada

来源：

PHYSICAL REVIEW D | 2011年 / 84卷 / 12期

基金：

美国国家科学基金会; 加拿大自然科学与工程研究理事会;

关键词：

MASS; X-1;

D O I：

10.1103/PhysRevD.84.124052

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We calibrate an effective-one-body (EOB) model to numerical-relativity simulations of mass ratios 1, 2, 3, 4, and 6, by maximizing phase and amplitude agreement of the leading (2, 2) mode and of the subleading modes (2, 1), (3, 3), (4, 4) and (5, 5). Aligning the calibrated EOB waveforms and the numerical waveforms at low frequency, the phase difference of the (2, 2) mode between model and numerical simulation remains below similar to 0.1 rad throughout the evolution for all mass ratios considered. The fractional amplitude difference at peak amplitude of the (2, 2) mode is 2% and grows to 12% during the ringdown. Using the Advanced LIGO noise curve we study the effectualness and measurement accuracy of the EOB model, and stress the relevance of modeling the higher-order modes for parameter estimation. We find that the effectualness, measured by the mismatch between the EOB and numerical-relativity polarizations which include only the (2, 2) mode, is smaller than 0.2% for binaries with total mass 20-200M(circle dot) and mass ratios 1, 2, 3, 4, and 6. When numerical-relativity polarizations contain the strongest seven modes, and stellar-mass black holes with masses less than 50M(circle dot) are considered, the mismatch for mass ratio 6 (1) can be as high as 7% (0.2%) when only the EOB (2, 2) mode is included, and an upper bound of the mismatch is 0.5% (0.07%) when all the four subleading EOB modes calibrated in this paper are taken into account. For binaries with intermediate-mass black holes with masses greater than 50M(circle dot) the mismatches are larger. We also determine for which signal-to-noise ratios the EOB model developed here can be used to measure binary parameters with systematic biases smaller than statistical errors due to detector noise.

引用

页数：26

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