Data-driven extraction, phenomenology, and modeling of eccentric harmonics in binary black hole merger waveforms
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Abstract
Newtonian and post-Newtonian (PN) calculations suggest that each spherical harmonic mode of the gravitational waveforms (radiation) emitted by eccentric binaries can be further decomposed into several eccentricity-induced modes (indexed by 𝑗=1 to 𝑗 =∞), referred to as eccentric harmonics. These harmonics exhibit monotonically time-varying amplitudes and instantaneous frequencies, unlike the full eccentric spherical harmonic modes. However, computing or extracting these harmonics is not straightforward in current numerical relativity simulations and eccentric waveform models. To address this, Patterson et al. [Identifying eccentricity in binary black hole mergers using a harmonic decomposition of the gravitational waveformPhys. Rev. D 111, 044073 (2025)] have developed a framework to extract the eccentric harmonics directly from effective-one-body formalism waveforms. In this paper, we build on the ideas presented in Patterson et al. and propose a data-driven framework, utilizing singular-value decomposition, that incorporates additional features based on PN intuition to ensure monotonicity in the extracted harmonics. We further demonstrate that the phase (frequency) of these harmonics is simply 𝑗𝜙𝜆+𝜙ecc (𝑗𝑓𝜆 +𝑓ecc), where 𝜙𝜆 (𝑓𝜆) is related to the secular orbital phase (frequency) and 𝜙ecc (𝑓ecc) is an additional phase (frequency) that only depends on the eccentricity. We also provide simple analytical fits to obtain the harmonics as a function of the mean anomaly. These relations may prove useful in constructing faithful models (such as [gwharmone: First data-driven surrogate for eccentric harmonics in binary black hole merger waveforms (to be published).]) that can be employed in cheap and efficient searches and parameter estimation of eccentric mergers. Our framework is modular and can be extended for any other eccentric waveform models or simulation frameworks. The framework is available through the gwminer package.
Copyright and License
© 2025 American Physical Society.
Acknowledgement
We thank Steve Fairhurst, Ben Patterson, Scott Field, Peter James Nee, Lucy Thomas, and Antoni Ramos-Buades for useful discussions and comments.
Funding
This research was supported in part by the National Science Foundation under Grant No. NSF PHY-2309135 and the Simons Foundation (Grant No. 216179, Lars Bildsten). Use was made of computational facilities purchased with funds from the National Science Foundation (Grant No. CNS-1725797) and administered by the Center for Scientific Computing (CSC). The CSC is supported by the California NanoSystems Institute and the Materials Research Science and Engineering Center (MRSEC; Grant No. NSF DMR 2308708) at University of California Santa Barbara. J. R. acknowledges support from the Sherman Fairchild Foundation. T. V. acknowledges support from NSF Grants No. 2012086 and No. 2309360, the Alfred P. Sloan Foundation through Grant No. FG-2023-20470, the U.S.-Israel Binational Science Foundation (BSF) through Grant No. 2022136, and the Hellman Family Faculty Fellowship.
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Additional details
Related works
- Is new version of
- Discussion Paper: arXiv:2504.12469 (arXiv)
Funding
- National Science Foundation
- PHY-2309135
- Simons Foundation
- 216179
- National Science Foundation
- CNS-1725797
- National Science Foundation
- DMR-2308708
- Sherman Fairchild Foundation
- National Science Foundation
- 2012086
- National Science Foundation
- 2309360
- Alfred P. Sloan Foundation
- FG-2023-20470
- United States-Israel Binational Science Foundation
- 2022136
- Hellman Foundation
Dates
- Accepted
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2025-07-30