Samurai project: Verifying the consistency of black-hole-binary waveforms for gravitational-wave detection

Hannam, M. D.; Husa, S.; Baker, John G.; Boyle, Michael; Bruegmann, Bernd; Chu, Tony; Dorband, Nils; Herrmann, Frank; Hinder, Ian; Kelly, Bernard; Kidder, Lawrence E.; Laguna, Pablo; Matthews, K.; Meter, James R. van; Pfeiffer, Harald P.; Pollney, Denis; Reisswig, Christian; Scheel, Mark A.; Shoemaker, D. M.

doi:10.1103/physrevd.79.084025

Cited by 76 publications

(94 citation statements)

References 181 publications

(225 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This code also supplies the total ADM energy M ADM of the system, as well as the individual "puncture ADM masses" M ADM,i , to very high precision. We note, however, that for highly spinning or boosted Bowen-Yorktype data, a measurable amount of radiation energy may be included in these puncture ADM masses, but then escape to infinity [8,[40][41][42]; thus the initial puncture ADM mass may not be the optimal measure of premerger black-hole mass. These quantities are also listed in Table I.…”

Section: Simulationsmentioning

confidence: 99%

“…The strongest radiation is produced just as the two black holes join to become one, and can only be fully understood through explicit numerical simulations. Since the first stable evolutions of black-hole-binary mergers [2][3][4][5], and after it was established that the gravitational waveforms from these evolutions were universal, and consistent across codes and methodologies [6][7][8], researchers have turned their attention to how the results of numerical relativity can most usefully be supplied to the gravitational-wave data-analysis community.…”

mentioning

confidence: 99%

See 1 more Smart Citation

Mergers of black-hole binaries with aligned spins: Waveform characteristics

et al. 2011

Self Cite

View full text Add to dashboard Cite

We conduct a descriptive analysis of the multipolar structure of gravitational-radiation waveforms from equal-mass aligned-spin mergers, following an approach first presented in the complementary context of nonspinning black holes of varying mass ratio [1]. We find that, as with the nonspinning mergers, the dominant waveform mode phases evolve together in lock-step through inspiral and merger, supporting the previous waveform description in terms of an adiabatically rigid rotator driving gravitational-wave emission -an implicit rotating source (IRS). We further apply the latetime merger-ringdown model for the rotational frequency introduced in [1], along with an improved amplitude model appropriate for the dominant (2, ±2) modes. This provides a quantitative description of the merger-ringdown waveforms, and suggests that the major features of these waveforms can be described with reference only to the intrinsic parameters associated with the state of the final black hole formed in the merger. We provide an explicit model for the merger-ringdown radiation, and demonstrate that this model agrees to fitting factors better than 95% with the original numerical waveforms for system masses above ∼ 150M⊙. This model may be directly applicable to gravitational-wave detection of intermediate-mass black hole mergers.

show abstract

Section: Simulationsmentioning

confidence: 99%

mentioning

confidence: 99%

Mergers of black-hole binaries with aligned spins: Waveform characteristics

et al. 2011

Self Cite

View full text Add to dashboard Cite

show abstract

“…The quantities T ℓm , δ ℓm , ρ ℓm , ρ J ℓm can be read from Eqs. (19), (20), (23), (25), (C1), (C4) and (C6) in Ref. [17], respectively.…”

Section: −1mentioning

confidence: 99%

“…[18][19][20][21][22][23][24][25]), we can compare in detail the EOB predictions with numerical results, and when necessary, introduce new features into the EOB model in order to improve its agreement with the numerical results. This is an important avenue to LIGO, GEO and Virgo template construction, as eventually thousands of waveform templates may be needed to detect the GW signal within the detector noise, and to extract astrophysical information from the observed waveform.…”

Section: Introductionmentioning

confidence: 99%

Effective-one-body waveforms calibrated to numerical relativity simulations: Coalescence of nonspinning, equal-mass black holes

et al. 2009

Self Cite

View full text Add to dashboard Cite

We calibrate the effective-one-body (EOB) model to an accurate numerical simulation of an equalmass, non-spinning binary black-hole coalescence produced by the Caltech-Cornell collaboration. Aligning the EOB and numerical waveforms at low frequency over a time interval of ∼ 1000M , and taking into account the uncertainties in the numerical simulation, we investigate the significance and degeneracy of the EOB adjustable parameters during inspiral, plunge and merger, and determine the minimum number of EOB adjustable parameters that achieves phase and amplitude agreements on the order of the numerical error. We find that phase and fractional amplitude differences between the numerical and EOB values of the dominant gravitational wave mode h22 can be reduced to 0.02 radians and 2%, respectively, until a time 20M before merger, and to 0.04 radians and 7%, respectively, at a time 20M after merger (during ringdown). Using LIGO, Enhanced LIGO and Advanced LIGO noise curves, we find that the overlap between the EOB and the numerical h22, maximized only over the initial phase and time of arrival, is larger than 0.999 for equal-mass binary black holes with total mass 30-150M⊙. In addition to the leading gravitational mode (2, 2), we compare the dominant subleading modes (4, 4) and (3, 2) for the inspiral and find phase and amplitude differences on the order of the numerical error. We also determine the mass-ratio dependence of one of the EOB adjustable parameters by calibrating to numerical inspiral waveforms for black-hole binaries with mass ratios 2:1 and 3:1. The results presented in this paper improve and extend recent successful attempts aimed at providing gravitational-wave data analysts the best analytical EOB model capable of interpolating accurate numerical simulations.

show abstract

“…These detectors are primarily sensitive to the oscillatory components of the GW signal, as most of the signal power lies in the lowest-order oscillatory modes of the radiation (for nearly circular orbits). More recently, successes in numerical relativity (NR) [45,46,47,48,49,50,51,52,53,54,55,56,57,58,59] have necessitated the need for accurate PN waveforms to compare with the results of binary black-hole (BH) merger simulations [60,61,62,63,64,65,66,67,68,69,70,71,5 This statement is only true for standard choices of the polarization triad (see Sec. II A).…”

Section: A What Is Gravitational-wave Memory?mentioning

confidence: 99%

Post-Newtonian corrections to the gravitational-wave memory for quasicircular, inspiralling compact binaries

2009

View full text Add to dashboard Cite

The Christodoulou memory is a nonlinear contribution to the gravitational-wave field that is sourced by the gravitational-wave stress-energy tensor. For quasicircular, inspiralling binaries, the Christodoulou memory produces a growing, nonoscillatory change in the gravitational-wave "plus" polarization, resulting in the permanent displacement of a pair of freely-falling test masses after the wave has passed. In addition to its nonoscillatory behavior, the Christodoulou memory is interesting because even though it originates from 2.5 post-Newtonian (PN) order multipole interactions, it affects the waveform at leading (Newtonian/quadrupole) order. The memory is also potentially detectable in binary black-hole mergers. While the oscillatory pieces of the gravitational-wave polarizations for quasicircular, inspiralling compact binaries have been computed to 3PN order, the memory contribution to the polarizations has only been calculated to leading order (the next-toleading order 0.5PN term has previously been shown to vanish). Here the calculation of the memory for quasicircular, inspiralling binaries is extended to 3PN order. While the angular dependence of the memory remains qualitatively unchanged, the PN correction terms tend to reduce the memory's magnitude. Explicit expressions are given for the memory contributions to the plus polarization and the spin-weighted spherical-harmonic modes of the metric and curvature perturbations. Combined with the recent results of Blanchet et al. [Class. Quantum Grav. 25, 165003 (2008)], this completes the waveform polarizations to 3PN order. This paper also discusses: (i) the difficulties in extracting the memory from numerical relativity simulations, (ii) other nonoscillatory effects that enter the waveform polarizations at high PN orders, and (iii) issues concerning the observability of the memory in gravitational-wave detectors.

show abstract

Samurai project: Verifying the consistency of black-hole-binary waveforms for gravitational-wave detection

Cited by 76 publications

References 181 publications

Mergers of black-hole binaries with aligned spins: Waveform characteristics

Mergers of black-hole binaries with aligned spins: Waveform characteristics

Effective-one-body waveforms calibrated to numerical relativity simulations: Coalescence of nonspinning, equal-mass black holes

Post-Newtonian corrections to the gravitational-wave memory for quasicircular, inspiralling compact binaries

Contact Info

Product

Resources

About