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Analytic systematics in next-generation of effective-one-body gravitational waveform models for future observations

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arxiv 2304.09662 v2 pith:IXEUFKVV submitted 2023-04-19 gr-qc

Alessandro Nagar , Piero Rettegno , Rossella Gamba , Simone Albanesi , Angelica Albertini , Sebastiano Bernuzzi This is my paper · ORCID
classification gr-qc
keywords waveformmodelmodelsanalyticbinariesblackconfigurationseffective-one-body
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abstract

The success of analytic waveform modeling within the effective-one-body (EOB) approach relies on the precise understanding of the physical importance of each technical element included in the model. The urgency of constructing progressively more sophisticated and complete waveform models (e.g. including spin precession and eccentricity) partly defocused the research from a careful comprehension of each building block (e.g. Hamiltonian, radiation reaction, ringdown attachment). Here we go back to the spirit of the first EOB works. We focus first on nonspinning, quasi-circular, black hole binaries and analyze systematically the mutual synergy between numerical relativity (NR) informed functions and the high post-Newtonian corrections (up to 5PN) to the EOB potentials. Our main finding is that it is essential to correctly control the noncircular part of the dynamics during the late plunge up to merger. We then improve the {\tt TEOBResumS-GIOTTO} waveform model for quasi-circular, spin-aligned black hole binaries. We obtain maximal EOB/NR unfaithfulness ${\bar{F}}^{\rm max}_{\rm EOBNR}\sim 10^{-3}$ (with Advanced LIGO noise and in the total mass range $10-200M_\odot$) for the dominant $\ell=m=2$ mode all over the 534 spin-aligned configurations available through the Simulating eXtreme Spacetime catalog. The model performance, also including higher modes, is then explored using the NR surrogates \nrsurqeight{} and \nrsurqfifteen, to validate it up to mass ratio $m_1/m_2=15$. We find that, over the set of configurations considered, more than $98\%$ of the total-mass-maximized unfaithfulness lie below the $3\%$ threshold when comparing to the surrogate models.

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Cited by 7 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Third post-Newtonian dynamics for eccentric orbits and aligned spins in the effective-one-body waveform model SEOBNRv5EHM

    gr-qc 2024-12 conditional novelty 7.0 of 10

    The authors obtain, for the first time, 3PN-accurate eccentric-orbit fluxes, radiation-reaction force, and waveform modes in the effective-one-body formalism, and use them to build the SEOBNRv5EHM inspiral model.

  2. Accurate waveforms for eccentric, aligned-spin binary black holes: The multipolar effective-one-body model SEOBNRv5EHM

    gr-qc 2024-12 conditional novelty 7.0 of 10

    SEOBNRv5EHM, a new effective-one-body waveform model with third-post-Newtonian eccentricity corrections, reaches a median 0.02% mismatch against eccentric numerical-relativity simulations, about an order of magnitude ...

  3. Can Eccentric Binary Black Hole Signals Mimic Gravitational-Wave Microlensing?

    gr-qc 2025-12 conditional novelty 6.0 of 10

    Eccentric BBH signals can masquerade as wave-optics microlensing in quasicircular analyses, but eccentric recovery templates break the degeneracy.

  4. Spinning Effective-to-Backwards One Body ($\texttt{SEBOB}$): combining Effective One-Body inspirals and Backwards One-Body merger-ringdowns for aligned spin black hole binaries

    gr-qc 2025-08 conditional novelty 6.0 of 10

    SEBOB combines an EOB inspiral with a BOB merger-ringdown to produce aligned-spin waveforms that match numerical relativity to about 2e-4 median mismatch, comparable to SEOBNRv5.

  5. Black-hole - neutron-star mergers: new numerical-relativity simulations and multipolar effective-one-body model with spin precession and eccentricity

    gr-qc 2025-06 conditional novelty 6.0 of 10

    A new catalog of 52 numerical-relativity BHNS merger simulations is used to calibrate TEOBResumS-Dalí, an improved effective-one-body waveform model with multipolar ringdown, spin precession, and eccentricity.

  6. Optimizing Neural Network Surrogate Models: Application to Black Hole Merger Remnants

    gr-qc 2025-01 conditional novelty 6.0 of 10

    A systematically optimized neural network surrogate for black-hole merger remnant properties, NRSur7dq4Remnant_NN, matches the accuracy of the GPR-based NRSur7dq4Remnant while evaluating up to 8 times faster on a CPU ...

  7. AthenaK simulations of the binary black hole merger GW150914

    gr-qc 2025-06 conditional novelty 5.0 of 10

    A new open-source GPU code, AthenaK, reproduces the GW150914 merger: remnant mass within 0.01%, spin within 0.02%, and waveform phase within about 0.35 radians of established simulations.

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