Numerical-relativity validation of effective-one-body waveforms in the intermediate-mass-ratio regime

Nagar, Alessandro; Healy, James; Lousto, Carlos O.; Bernuzzi, Sebastiano; Albertini, Angelica

doi:10.48550/arxiv.2202.05643

Cited by 9 publications

(30 citation statements)

References 89 publications

(153 reference statements)

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“…This was already pointed out in Ref. [68], thanks to a specific EOB/NR comparison involving the standard TEOBResumS and a recently obtained q = 15 NR simulation [69]. The inclusion of more testmass terms in the resummed flux (notably up to 22PN accuracy [70]) brings a much closer agreement between analytical and numerical fluxes in the test-mass limit.…”

Section: Discussionsupporting

confidence: 63%

Towards a gravitational self force-informed effective-one-body waveform model for nonprecessing, eccentric, large-mass-ratio inspirals

Nagar¹,

Albanesi²

2022

Preprint

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Building upon several recent advances in the development of effective-one-body models for spinaligned eccentric binaries with individual masses (m1, m2) we introduce a new EOB waveform model that aims at describing inspiralling binaries in the large mass-ratio regime, m1 m2. The model exploits the current state-of-the-art TEOBResumS-DALI model for eccentric binaries, but the standard EOB potentials (A, D, Q), informed by Numerical Relativity (NR) simulations, are replaced with the corresponding functions that are linear in the symmetric mass ratio ν ≡ m1m2/(m1 + m2) 2 taken at 8.5PN accuracy. To improve their strong-field behavior, these functions are: (i) suitably factorized and resummed using Padé approximants and (ii) additionally effectively informed to state-of-the-art numerical results obtained by gravitational self-force theory (GSF). For simplicity, the spin-sector of the model is taken to be the one of TEOBResumS-DALI, though removing the NR-informed spinorbit effective corrections. We propose the current GSF-informed EOB framework as a conceptually complete analytical tool to generate waveforms for eccentric Extreme (and Intermediate) Mass Ratio Inspirals for future gravitational wave detectors.

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Section: Discussionsupporting

confidence: 63%

Towards a gravitational self force-informed effective-one-body waveform model for nonprecessing, eccentric, large-mass-ratio inspirals

Nagar¹,

Albanesi²

2022

Preprint

Self Cite

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“…Note however that the model was found to perform consistently with NR also for large mass ratios, up to the intermediate massratio regime[37].…”

mentioning

confidence: 74%

“…VA of Ref. [37]. We remind the reader that the notation 3 +19 PN means that the standard 3PN-accurate terms in the ρ ℓm 's (that depend 2 In particular, setting the radial radiation reaction force to zero, Fr = 0, as is the case for the native quasi-circular TEOBResumS model.…”

Section: B Waveform and Radiation Reactionmentioning

confidence: 99%

Comparing second-order gravitational self-force and effective one body waveforms from inspiralling, quasicircular and nonspinning black hole binaries. II. The large-mass-ratio case

Albertini

Nagar²,

Pound³

et al. 2022

Phys. Rev. D

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We compare recently computed waveforms from second-order gravitational self-force (GSF) theory to those generated by a new, GSF-informed, effective one body (EOB) waveform model for (spinaligned, eccentric) inspiralling black hole binaries with large mass ratios. We focus on quasi-circular, nonspinning, configurations and perform detailed GSF/EOB waveform phasing comparisons, either in the time domain or via the gauge-invariant dimensionless function Qω ≡ ω 2 / ω, where ω is the gravitational wave frequency. The inclusion of high-PN test-mass terms within the EOB radiation reaction (notably, up to 22PN) is crucial to achieve an EOB/GSF phasing agreement below 1 rad up to the end of the inspiral for mass ratios up to 500. For larger mass ratios, up to 5 × 10 4 , the contribution of horizon absorption becomes more and more important and needs to be accurately modeled. Our results indicate that our GSF-informed EOB waveform model is a promising tool to describe waveforms generated by either intermediate or extreme mass ratio inspirals for future gravitational wave detectors.

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“…These mass ratios are chosen for consistency with Ref. [14], that presents direct EOB/NR phasing comparisons in the IMR regime using the recent, breakthrough NR simulations of Refs. [19] and [13].…”

Section: B Eob/gsf Comparisons For Intermediate-mass-ratio Binaries Q...mentioning

confidence: 99%

Comparing second-order gravitational self-force, numerical relativity, and effective one body waveforms from inspiralling, quasicircular, and nonspinning black hole binaries

Albertini

Nagar²,

Pound³

et al. 2022

Phys. Rev. D

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We present the first systematic comparison between gravitational waveforms emitted by inspiralling, quasi-circular and nonspinning black hole binaries computed with three different approaches: second-order gravitational self-force (2GSF) theory, as implemented in the 1PAT1 model; numerical relativity (NR), as implemented by the SXS collaboration; and the effective one body (EOB) formalism, as implemented in the TEOBResumS waveform model. To compare the models we use both a standard, time-domain waveform alignment and a gauge-invariant analysis based on the dimensionless function Qω(ω) ≡ ω 2 / ω, where ω is the gravitational wave frequency. We analyse the domain of validity of the 1PAT1 model, deriving error estimates and showing that the effects of the final transition to plunge, which the model neglects, extend over a significantly larger frequency interval than one might expect. Restricting to the inspiral regime, we find that, while for mass ratios q = m1/m2 ≤ 10 TEOBResumS is largely indistinguishable from NR, 1PAT1 has a significant dephasing ≳ 1 rad; conversely, for q ≳ 100, 1PAT1 is estimated to have phase errors < 0.1 rad on a large frequency interval, while TEOBResumS develops phase differences ≳ 1 rad with it. Most crucially, on that same large frequency interval we find good agreement between TEOBResumS and 1PAT1 in the intermediate regime 15 ≲ q ≲ 64, with < 0.5 rad dephasing between them. A simple modification to the TEOBResumS flux further improves this agreement for q ≳ 30, reducing the dephasing to ≈ 0.27 rad even at q = 128. While our analysis points to the need for more highly accurate, long-inspiral, NR simulations for q ≳ 15 to precisely quantify the accuracy of EOB/2GSF waveforms, we can clearly identify the primary sources of error and routes to improvement of each model. In particular, our results pave the way for the construction of GSF-informed EOB models for both intermediate and extreme mass ratio inspirals for the next generation of gravitational wave detectors.

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Numerical-relativity validation of effective-one-body waveforms in the intermediate-mass-ratio regime

Cited by 9 publications

References 89 publications

Towards a gravitational self force-informed effective-one-body waveform model for nonprecessing, eccentric, large-mass-ratio inspirals

Towards a gravitational self force-informed effective-one-body waveform model for nonprecessing, eccentric, large-mass-ratio inspirals

Comparing second-order gravitational self-force and effective one body waveforms from inspiralling, quasicircular and nonspinning black hole binaries. II. The large-mass-ratio case

Comparing second-order gravitational self-force, numerical relativity, and effective one body waveforms from inspiralling, quasicircular, and nonspinning black hole binaries

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