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

Kelly, Bernard; Baker, John G.; Boggs, William D.; McWilliams, S. T.; Centrella, Joan

doi:10.1103/physrevd.84.084009

Cited by 30 publications

(44 citation statements)

References 115 publications

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“…Under this assumption, we complement the inspiral evolution of the ax-model with a noneccentric merger waveform. This stand-alone merger waveform is constructed by calibrating the IRS model introduced by Kelly et al [78] with a catalog of NR simulations [86] obtained with the Spectral Einstein Code [87]. These simulations describe nonspinning, quasicircular compact binary systems with mass ratios between q ¼ 2.5 and q ¼ 10 [86,88].…”

Section: E Merger and Ringdown Evolutionmentioning

confidence: 99%

“…The IRS model encapsulates the evolution of the orbital frequency evolution, ωðtÞ, and the waveform amplitude, AðtÞ, using the prescription [51,78,89,90] ωðtÞ ¼ ω QNM ð1 −fÞ; ð19Þ…”

Section: E Merger and Ringdown Evolutionmentioning

confidence: 99%

“…(3) To further improve phase accuracy especially for unequal-mass systems, the 3PN accurate inspiral evolution for eccentric systems is corrected by including up to 6PN terms both for the energy flux of quasicircular binaries and gravitational self-force corrections to the binding energy of compact binaries at first order in the symmetric mass ratio η. (4) We combine the aforementioned enhanced inspiral evolution with a merger and ringdown treatment using the implicit rotating source (IRS) formalism [78], fitted against NR simulations up to mass ratio 10. The eccentric model we develop in this article is the first model in the literature that combines all these features, and makes it a powerful tool to explore the detection of eccentric signals with aLIGO.…”

Section: Introductionmentioning

confidence: 99%

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Complete waveform model for compact binaries on eccentric orbits

et al. 2017

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We present a time domain waveform model that describes the inspiral, merger and ringdown of compact binary systems whose components are nonspinning, and which evolve on orbits with low to moderate eccentricity. The inspiral evolution is described using third-order post-Newtonian equations both for the equations of motion of the binary, and its far-zone radiation field. This latter component also includes instantaneous, tails and tails-of-tails contributions, and a contribution due to nonlinear memory. This framework reduces to the post-Newtonian approximant TaylorT4 at third postNewtonian order in the zero-eccentricity limit. To improve phase accuracy, we also incorporate higher-order post-Newtonian corrections for the energy flux of quasicircular binaries and gravitational self-force corrections to the binding energy of compact binaries. This enhanced prescription for the inspiral evolution is combined with a fully analytical prescription for the merger-ringdown evolution constructed using a catalog of numerical relativity simulations. We show that this inspiral-mergerringdown waveform model reproduces the effective-one-body model of Ref. [Y. Pan et al., Phys. Rev. D 89, 061501 (2014).] for quasicircular black hole binaries with mass ratios between 1 to 15 in the zero-eccentricity limit over a wide range of the parameter space under consideration. Using a set of eccentric numerical relativity simulations, not used during calibration, we show that our new eccentric model reproduces the true features of eccentric compact binary coalescence throughout merger. We use this model to show that the gravitational-wave transients GW150914 and GW151226 can be effectively recovered with template banks of quasicircular, spin-aligned waveforms if the eccentricity e 0 of these systems when they enter the aLIGO band at a gravitational-wave frequency of 14 Hz satisfies e GW150914 0 ≤ 0.15 and e GW151226 0 ≤ 0.1. We also find that varying the spin combinations of the quasicircular, spin-aligned template waveforms does not improve the recovery of nonspinning, eccentric signals when e 0 ≥ 0.1. This suggests that these two signal manifolds are predominantly orthogonal.

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Section: E Merger and Ringdown Evolutionmentioning

confidence: 99%

Section: E Merger and Ringdown Evolutionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Complete waveform model for compact binaries on eccentric orbits

et al. 2017

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“…On the contrary, in the case of comparable-mass BH binaries, mode mixing seems less ubiquitous, and so far it has only been seen in the (3,2) mode [49][50][51][52][53][54][55]. For this reason, in the past, when modeling the ringdown of the ðl; mÞ mode in the EOB approach, one could simply use the ðl; m; nÞ QNMs.…”

Section: Quasinormal-mode Mixing In Ringdown Teukolsky Waveforms Amentioning

confidence: 99%

Small mass plunging into a Kerr black hole: Anatomy of the inspiral-merger-ringdown waveforms

et al. 2014

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We numerically solve the Teukolsky equation in the time domain to obtain the gravitational-wave emission of a small mass inspiraling and plunging into the equatorial plane of a Kerr black hole. We account for the dissipation of orbital energy using the Teukolsky frequency-domain gravitational-wave fluxes for circular, equatorial orbits, down to the light-ring. We consider Kerr spins −0.99 ≤ q ≤ 0.99, and compute the inspiral-merger-ringdown (2,2), (2,1), (3,3), (3,2), (4,4), and (5,5) modes. We study the largespin regime, and find a great simplicity in the merger waveforms, thanks to the extremely circular character of the plunging orbits. We also quantitatively examine the mixing of quasinormal modes during the ringdown, which induces complicated amplitude and frequency modulations in the waveforms. Finally, we explain how the study of small mass-ratio black-hole binaries helps extending effective-one-body models for comparable-mass, spinning black-hole binaries to any mass ratio and spin magnitude.

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“…Therefore, for aligned spins, the best-match parameters are shifted to increase the number of inspiral cycles while reducing the number of late-inspiral-merger cycles in the template (which increasing η, decreasing χ BH , and simultaneously increasing the total mass will do), in order to accumulate coherent SNR from the inspiral while minimizing the incoherent contribution from the late-inspiral cycles. On the other hand, antialigned component spins lead to sharper frequency evolution close to merger [92], and therefore are difficult to mimic by PN waveforms with shifted parameters. Therefore, the best match that PN models get is with the short early inspiral itself which (i) does not yield as high fitting factors, and (ii) does not require as much shifting of the spin/mass-ratio parameters from the true value.…”

Section: Effectualness and Parameter Biasmentioning

confidence: 99%

Accuracy and precision of gravitational-wave models of inspiraling neutron star-black hole binaries with spin: Comparison with matter-free numerical relativity in the low-frequency regime

et al. 2015

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Coalescing binaries of neutron stars and black holes are one of the most important sources of gravitational waves for the upcoming network of ground-based detectors. Detection and extraction of astrophysical information from gravitational-wave signals requires accurate waveform models. The effective-one-body and other phenomenological models interpolate between analytic results and numerical relativity simulations, that typically span Oð10Þ orbits before coalescence. In this paper we study the faithfulness of these models for neutron star-black hole binaries. We investigate their accuracy using new numerical relativity (NR) simulations that span 36-88 orbits, with mass ratios q and black hole spins χ BH of ðq; χ BH Þ ¼ ð7; AE0.4Þ; ð7; AE0.6Þ, and ð5; −0.9Þ. These simulations were performed treating the neutron star as a low-mass black hole, ignoring its matter effects. We find that (i) the recently published SEOBNRv1 and SEOBNRv2 models of the effective-one-body family disagree with each other (mismatches of a few percent) for black hole spins χ BH ≥ 0.5 or χ BH ≤ −0.3, with waveform mismatch accumulating during early inspiral; (ii) comparison with numerical waveforms indicates that this disagreement is due to phasing errors of SEOBNRv1, with SEOBNRv2 in good agreement with all of our simulations; (iii) phenomenological waveforms agree with SEOBNRv2 only for comparable-mass low-spin binaries, with overlaps below 0.7 elsewhere in the neutron star-black hole binary parameter space; (iv) comparison with numerical waveforms shows that most of this model's dephasing accumulates near the frequency interval where it switches to a phenomenological phasing prescription; and finally (v) both SEOBNR and post-Newtonian models are effectual for neutron star-black hole systems, but post-Newtonian waveforms will give a significant bias in parameter recovery. Our results suggest that future gravitational-wave detection searches and parameter estimation efforts would benefit from using SEOBNRv2 waveform templates when focused on neutron star-black hole systems with q ≲ 7 and χ BH ≈ ½−0.9; þ0.6. For larger black hole spins and/or binary mass ratios, we recommend the models be further investigated as NR simulations in that region of the parameter space become available.

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

Cited by 30 publications

References 115 publications

Complete waveform model for compact binaries on eccentric orbits

Complete waveform model for compact binaries on eccentric orbits

Small mass plunging into a Kerr black hole: Anatomy of the inspiral-merger-ringdown waveforms

Accuracy and precision of gravitational-wave models of inspiraling neutron star-black hole binaries with spin: Comparison with matter-free numerical relativity in the low-frequency regime

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