Inferring eccentricity evolution from observations of coalescing binary black holes

Bonino, Alice; Gamba, R.; Schmidt, P.; Nagar, Alessandro; Pratten, G.; Breschi, M.; Rettegno, P.; Bernuzzi, Sebastiano

doi:10.48550/arxiv.2207.10474

Cited by 2 publications

(2 citation statements)

References 61 publications

(118 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The definition of eccentricity could potentially be disentangled from other features of the waveform by measuring the eccentricity directly from its frequency evolution. The exploration of a standardized eccentricity parameter that could be used to compare measurements across different models is currently underway (Shaikh et al 2022, in preparation;Bonino et al 2022).…”

Section: Discussionmentioning

confidence: 99%

A Rosetta Stone for Eccentric Gravitational Waveform Models

Knee

Romero-Shaw

Lasky

et al. 2022

ApJ

View full text Add to dashboard Cite

Orbital eccentricity is a key signature of dynamical binary black hole formation. The gravitational waves from a coalescing binary contain information about its orbital eccentricity, which may be measured if the binary retains sufficient eccentricity near merger. Dedicated waveforms are required to measure eccentricity. Several models have been put forward, and show good agreement with numerical relativity at the level of a few percent or better. However, there are multiple ways to define eccentricity for inspiralling systems, and different models internally use different definitions of eccentricity, making it difficult to compare eccentricity measurements directly. In this work, we systematically compare two eccentric waveform models, SEOBNRE and TEOBResumS, by developing a framework to translate between different definitions of eccentricity. This mapping is constructed by minimizing the relative mismatch between the two models over eccentricity and reference frequency, before evolving the eccentricity of one model to the same reference frequency as the other model. We show that for a given value of eccentricity passed to SEOBNRE, one must input a 20%–50% smaller value of eccentricity to TEOBResumS in order to obtain a waveform with the same empirical eccentricity. We verify this mapping by repeating our analysis for eccentric numerical relativity simulations, demonstrating that TEOBResumS reports a correspondingly smaller value of eccentricity than SEOBNRE.

show abstract

Section: Discussionmentioning

confidence: 99%

A Rosetta Stone for Eccentric Gravitational Waveform Models

Knee

Romero-Shaw

Lasky

et al. 2022

ApJ

View full text Add to dashboard Cite

show abstract

“…[43]. The model builds upon the spin-aligned, eccentric TEOBResumS model, the TEOBResumS-DALI [45][46][47], but the low-PN accurate, NRinformed EOB potentials are replaced by the 1GSFinformed ones. More precisely, the potentials (A, D, Q) at linear order in ν formally read…”

Section: A the Hamiltonian: A Remindermentioning

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

View full text Add to dashboard Cite

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.

show abstract

Inferring eccentricity evolution from observations of coalescing binary black holes

Cited by 2 publications

References 61 publications

A Rosetta Stone for Eccentric Gravitational Waveform Models

A Rosetta Stone for Eccentric Gravitational Waveform Models

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

Contact Info

Product

Resources

About