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

By Yi Pan, A. Buonanno, M. Boyle, L. Buchman, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel. 2011

183 citations recorded by the source corpus.

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 ∼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_⊙ 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_⊙ 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_⊙ 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.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/494f9bd438dd07c733eb15b0402ac34c3848b355

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In Astronomy and Astrophysics

Citations in the corpus

COMPACT BINARY MERGER RATES: COMPARISON WITH LIGO/VIRGO UPPER LIMITS (2015, methodology): “We have verified explicitly that we obtain essentially identical rate estimates using an effective-one-body waveform model (more specifically, EOBNRv2; Pan et al. 2011).”
Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, methodology): ““Complete” waveforms can be designed by stitching together analytical PN waveforms for the early inspiral with a (semi)phenomenologically described merger and ring-down phase (Damour et al., 2011, Pan et al., 2011, Santamaría et al., 2010), calibrated against available numerical data.”
The evolution of massive black holes and their spins in their galactic hosts (2012, methodology): “…(see for instance the effective-one-body approach, e.g. Buonanno & Damour (1999); Damour, Jaranowski, & Schäfer (2008); Barausse & Buonanno (2010); Pan et al. (2011), or the hybrid waveforms, e.g. Santamarı́a et al. (2010)), the kick velocity (Baker et al. 2007, 2008; van Meter et al. 2010;…”
Surrogate model of hybridized numerical relativity binary black hole waveforms (2018, methodology): “Several inspiral-merger-ringdown waveform models [14,15,20,21] that include nonquadrupole modes have been developed in recent years; however, compared to those models we show an improved accuracy and we include more modes.”