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A quadrupole-based EOB flux and mode-mixing model cuts dephasing for extreme-mass-ratio black-hole binaries by up to an order of magnitude.

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2026-07-15 14:25 UTC pith:6XGK357T

load-bearing objection Solid, usable upgrade to SEOBNR in the test-mass limit: Q-factorized flux plus explicit mode-mixing give clear dephasing gains, with residual near-extremal softness already flagged by the authors. the 2 major comments →

arxiv 2603.05601 v1 pith:6XGK357T submitted 2026-03-05 gr-qc

Advancing the Effective-One-Body Framework in the Test-Mass Limit

Nami Nishimura , Alessandra Buonanno , Guglielmo Faggioli , Maarten van de Meent , Gaurav Khanna This is my paper
classification gr-qc PACS 04.30.Db04.25.Nx04.70.Bw
keywords effective-one-bodytest-mass limitextreme mass-ratio inspiralsgravitational-wave fluxhorizon absorptionmode mixingquasi-normal modesbinary black holes
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper builds SEOB-TML, an effective-one-body waveform model specialized for the extreme mass-ratio (test-mass) limit of quasi-circular, spin-aligned black-hole binaries. Instead of summing dozens of multipoles, it maps the entire energy flux—including energy absorbed by the horizon—onto a single quadrupole (2,2) baseline corrected by a high-order polynomial. Traditional next-to-quasicircular corrections are replaced by a flexible hyperbolic ansatz that lets each multipole attach to the ringdown at its own physically motivated time, and quasi-normal-mode coefficients extracted from Teukolsky waveforms are used to capture the amplitude and frequency modulations that appear when the orbital frequency reverses. The (2,0) memory mode is also included for the first time in this family. Against numerical Teukolsky benchmarks the model reduces accumulated phase error from several radians to a few tenths of a radian over hundreds of gravitational-wave cycles and removes spurious peaks near merger. The practical payoff is a computationally cheap, high-fidelity late-inspiral–merger–ringdown waveform usable for extreme- and intermediate-mass-ratio systems that future space- and ground-based detectors will see.

Core claim

SEOB-TML produces highly accurate late inspiral–merger–ringdown waveforms in the test-mass limit by combining a quadrupole-factorized energy flux (including horizon absorption) with a mode-dependent phenomenological attachment and explicit quasi-normal-mode mixing; relative to SEOBNRv5HM the accumulated dephasing drops by factors of five to ten or more across non-spinning, prograde and retrograde spins while near-merger residuals fall by an order of magnitude.

What carries the argument

The Q-factorized flux: the total energy flux (infinity plus horizon) is written as the factorized (2,2) mode multiplied by a fourth-power polynomial whose coefficients are fixed by matching the circular-orbit post-Newtonian expansion up to 9 PN (horizon term to 6.5 PN); this single baseline already encodes the higher multipoles that would otherwise require an expensive mode sum.

Load-bearing premise

The 9 PN quadrupole-factorized flux and a single phenomenological activation function remain accurate once the black-hole spin becomes near-extremal or highly retrograde, regimes where the paper itself already sees fractional flux errors of tens of percent and late-time frequency drifts that the ansatz cannot fully capture.

What would settle it

Generate a new high-accuracy Teukolsky waveform for a near-extremal prograde spin (a greater than or equal to 0.95) or a highly retrograde spin (a less than or equal to –0.95) and measure whether the SEOB-TML (2,2) phase residual after a few hundred cycles stays below one radian; if it climbs back to several radians the flux and activation assumptions fail.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 4 minor

Summary. The manuscript presents SEOB-TML, an EOB model specialized to the test-mass limit for quasi-circular, spin-aligned binaries. Its main technical ingredients are: (i) a quadrupole-factorized (Q-factorized) radiation-reaction flux that maps the total energy flux (infinity plus horizon absorption) onto a single (2,2) baseline multiplied by a 9PN polynomial β^{4}(x) (Eqs. 3.14–3.15, 3.26–3.27); (ii) replacement of NQC corrections by a mode-dependent hyperbolic phenomenological ansatz for the late inspiral-plunge (Eqs. 4.6–4.7) together with flexible attachment times (Eq. 4.2); (iii) explicit inclusion of mode-mixing via QNM coefficients extracted with qnmfinder, activated by a refined window function (Eq. 6.2); and (iv) a full IMR construction of the (2,0) mode. Direct comparisons against independent FD/TD Teukolsky data show order-of-magnitude reductions in fractional flux error (Figs. 1–4, Table I) and accumulated dephasing relative to SEOBNRv5HM (e.g., 7.02 rad → 0.91 rad for a=0.9 over ~125 cycles; Figs. 18–20, 26–27).

Significance. If the reported gains hold under independent scrutiny, the work supplies a concrete, computationally efficient route for bringing EOB models into the EMRI/IMRI regime that next-generation detectors will probe. The Q-factorized flux is a genuine architectural simplification: it absorbs higher multipoles without an expensive ℓ_max~10–30 sum while remaining competitive with (and often superior to) the traditional M-factorized flux at the same PN order. Explicit use of qnmfinder-extracted QNM amplitudes for retrograde mixing, rather than purely phenomenological coefficients, is a methodological advance that can be reused for eccentric or precessing extensions. The paper is transparent about residual degradation near a≳0.95 and for highly retrograde late-time frequency drifts, which strengthens rather than weakens the claim for the bulk of the parameter space |a|≲0.9.

major comments (2)
  1. The free-parameter budget is large (Δt_ℓm^Ωpeak, γ/λ, c_i^ℓm, d_i^ℓm, A_ℓ–m0/A_ℓm0 ratios, and the three activation parameters in Eq. 6.2) and all of these coefficients are obtained by least-squares fits to the same Teukolsky waveforms later used as the accuracy benchmark. While the flux polynomials themselves are fixed by PN matching and are therefore non-circular, the waveform-sector gains (especially the near-merger residual reductions in Figs. 18–20) cannot be cleanly separated from this calibration. A short hold-out test—e.g., coefficients fitted on a subset of spins and evaluated on the remaining spins—would make the generalization claim quantitative rather than visual.
  2. Appendix A and Table I document that the total Q-factorized flux reaches ~70 % fractional error at the ISCO for a=0.959, driven by the horizon term (Fig. 24). The abstract and Sec. IX still describe the framework as generating “highly accurate” late IMR waveforms for extreme-mass-ratio systems without an explicit validity domain. The manuscript should state a clear recommended range (e.g., |a|≲0.9 or a≲0.95) and, if possible, sketch the higher-PN or numerically calibrated correction to α(x) that the authors themselves propose in Appendix A.
minor comments (4)
  1. Eq. (3.15) and the surrounding text use both β(x) and α(x) for the infinity and horizon multiplicative factors; the notation is consistent once introduced, but a single sentence early in Sec. III B clarifying the two symbols would help the reader.
  2. Figure 5 caption and the text of Sec. IV A refer to spin-independent offsets of 2.5M and 3.5M for the (3,2) and (4,3) attachment times; a short table of the actual fitted Δt_ℓm^Ωpeak values (or a statement that they are available in the supplemental notebook) would improve reproducibility.
  3. The (2,0) construction (Sec. VIII) relies on a Hilbert transform whose post-merger oscillations are acknowledged as possible artifacts; a brief quantitative comparison of the complexified amplitude against a pure real-valued ansatz would clarify whether the residual discrepancy for a=0.9 is physical or numerical.
  4. Typographical: “Gravitaional” in the first author affiliation; occasional missing spaces around “SEOB-TML” and “SEOBNRv5HM”; “qnmfinder” is sometimes italicized and sometimes not.

Circularity Check

5 steps flagged

Waveform-level performance claims rest partly on a calibration loop: free coefficients (attachment times, hyperbolic γ/λ, merger-RD c_i, QNM ratios, activation parameters) are least-squares fitted to the same Teukolsky waveforms later used as the accuracy benchmark.

specific steps
  1. fitted input called prediction [Sec. IV A, Eq. (4.4) and surrounding text]
    "To determine Δt_Ωpeak, we extract the mode-dependent matching times from TD Teukolsky waveforms and the peak orbital frequency times from trajectories computed employing FD Teukolsky fluxes. These values are then interpolated as a function of spin."

    Attachment times that define the inspiral-plunge / merger-RD split are fitted directly to the same Teukolsky waveforms later used as the accuracy benchmark. Once Δt is fixed, the model is forced to attach at the numerically observed peak (or Ω=0 crossing), so residual agreement near attachment is partly by construction.

  2. fitted input called prediction [Sec. IV B, Eqs. (4.6)–(4.10) and Fig. 7]
    "The phenomenological coefficients a_i and b_i are fixed by enforcing continuity and differentiability with the EOB inspiral waveform and with numerical input values, specifically the amplitude and frequency data extracted from Teukolsky waveforms. … By allowing γ and λ to vary, the model captures the (2,1) mode more accurately … The optimized coefficients are subsequently interpolated and fitted as a function of spin for implementation in the model."

    The hyperbolic ansatz that replaces NQC corrections is collocation-matched at t_cut, t_cp and t_match to Teukolsky amplitude/frequency values, and the free steepness parameters γ,λ are least-squares fitted to the same data. Late-inspiral residuals are therefore statistically forced rather than predicted.

  3. fitted input called prediction [Sec. V A, after Eqs. (5.4)–(5.5)]
    "The free parameters c_i^{lm} and d_i^{lm} are first obtained from least-squares fits to individual Teukolsky waveforms and then interpolated across spin a using rational function fits."

    Merger-RD free coefficients that control amplitude and phase evolution after attachment are fitted to the identical Teukolsky waveforms later used for residual comparisons (Figs. 8, 11–17). Agreement in the ringdown sector is therefore partly by construction.

  4. fitted input called prediction [Sec. V C / Sec. VI, Figs. 9–10 and Eq. (6.1)]
    "When incorporating this extracted QNM information into our model, we must fit not only the parameters c_1lm, c_2lm, d_1lm and d_2lm from Eqs. (5.2) and (5.3), but also the ratio of A_{−m0}/A_m0 across the range of spin values. … Consequently, we interpolate these ratios across the spin parameter space by fitting them with rational functions."

    QNM amplitude ratios that control the strength of retrograde (and spheroidal) mixing are extracted via qnmfinder from the same Teukolsky waveforms and then re-inserted into the ansatz. The characteristic amplitude/frequency modulations that the paper claims to capture are therefore re-injected rather than independently predicted.

  5. fitted input called prediction [Sec. VI A, after Eq. (6.2)]
    "Finally, the parameters ( au0, au1, au2), introduced in the activation function defined in Eq. (6.2) are tuned for each mode to control the onset and steepness of the activation. For the (2,2) mode, for example, we use ( au0, au1, au2)=(20,7.5,7.5) for a≥−0.9, while for a<−0.9 we increase au0 to 25 and au1 to 10 …"

    The phenomenological activation function that turns on retrograde QNMs is hand-tuned (and spin-dependent) against the same Teukolsky data. Early-ringdown residuals for highly retrograde spins are therefore partly absorbed by construction into the free parameters of heta( au).

full rationale

The Q-factorized flux itself is not circular: its polynomial coefficients are fixed by order-by-order matching to independent high-order PN expansions (9PN infinity, 6.5PN horizon) and then validated against FD Teukolsky fluxes that are not used in the matching (Figs. 1–4, Table I). That part of the derivation is self-contained and predictive. However, the strongest claim—order-of-magnitude dephasing reduction and improved near-merger reconstruction relative to SEOBNRv5HM—is demonstrated exclusively on TD Teukolsky waveforms to which the model has already been calibrated. Attachment offsets Δt_Ωpeak, hyperbolic γ/λ, merger-RD free parameters c_i, QNM amplitude ratios A_−m0/A_m0, and activation-function parameters ( au0, au1, au2) are all obtained by least-squares fits or interpolation against the identical Teukolsky data later shown in Figs. 18–20 and 26–27. Once those coefficients are fixed, residual agreement is partly by construction. The paper is transparent about residual degradation at |a|≳0.95, so the circularity is partial rather than total; the flux improvement remains independent content. Score 5 reflects that the central waveform-level claim is statistically forced by the calibration loop while the dynamical flux advance is not.

Axiom & Free-Parameter Ledger

6 free parameters · 4 axioms · 2 invented entities

The model rests on the standard EOB mapping of the two-body problem onto a deformed Kerr geodesic, on the Teukolsky equation for the numerical benchmarks, and on a large set of phenomenological coefficients that are fitted to those benchmarks. No new physical entities are postulated; the free parameters are the usual calibration knobs of waveform models.

free parameters (6)
  • Δt_lm^Ωpeak (mode- and spin-dependent attachment offsets)
    Interpolated from Teukolsky peak times; frozen for a>0.95 to avoid unreliable peak locations.
  • γ, λ (hyperbolic-ansatz steepness parameters)
    Fitted mode-by-mode to late-plunge Teukolsky amplitude and frequency; especially important for (2,1) at large negative spin.
  • c1^lm, c2^lm, d1^lm, d2^lm (merger-RD amplitude and phase coefficients)
    Least-squares fits to individual Teukolsky waveforms, then rational-function interpolated in spin.
  • A_ℓ–m0 / A_ℓm0 (retrograde-to-prograde QNM amplitude ratios)
    Extracted by qnmfinder and fitted with rational functions across spin.
  • τ0, τ1, τ2 (activation-function parameters in Eq. 6.2)
    Tuned by hand for each mode and spin regime to control onset of mixing.
  • a4 (extra amplitude coefficient in hyperbolic ansatz)
    Introduced to allow non-zero derivative at non-peak attachment times; set to zero when attachment coincides with the peak.
axioms (4)
  • domain assumption The two-body dynamics in the test-mass limit reduce to a Kerr geodesic plus radiation-reaction force computed from the energy flux.
    Standard EOB premise used throughout Sec. III; higher-order self-force corrections are set to zero.
  • domain assumption The Teukolsky equation with a point-particle source supplies the exact leading-order gravitational waveform and fluxes.
    All numerical benchmarks (ModGEMS fluxes, hyperboloidal time-domain waveforms) rest on this equation.
  • ad hoc to paper A single (2,2) mode multiplied by a 9PN polynomial can absorb the contribution of all higher multipoles to the total flux.
    The defining assumption of the Q-factorized prescription (Eq. 3.14); validated a posteriori but not derived from first principles.
  • ad hoc to paper Mode mixing after orbital-frequency reversal is adequately captured by a linear superposition of the fundamental prograde and retrograde QNMs activated by a single phenomenological window.
    Eqs. 6.1–6.4; the paper notes residual early-time discrepancies for |a|≳0.9.
invented entities (2)
  • Q-factorized flux (total energy flux mapped onto a single (2,2) baseline times β^4(x)) no independent evidence
    purpose: Eliminate expensive multipole sums while retaining high accuracy in the strong-field regime.
    New factorization introduced in Sec. III B; independent evidence is the comparison to Teukolsky fluxes, but the construction itself is postulated.
  • Refined activation function f(τ) (Eq. 6.2) that enforces vanishing value and derivative at attachment while supplying extra phase freedom no independent evidence
    purpose: Smoothly turn on retrograde and spheroidal-mixing QNMs without spoiling C1 continuity.
    Phenomenological device introduced to improve on the earlier sigmoid of Taracchini et al.; no external falsifiable prediction.

pith-pipeline@v1.1.0-grok45 · 58152 in / 3334 out tokens · 35726 ms · 2026-07-15T14:25:26.818680+00:00 · methodology

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read the original abstract

We present SEOB-TML, an enhanced effective-one-body (EOB) framework for the test-mass limit, optimized for quasi-circular, spin-aligned binary black holes. On the dynamical side, we introduce a quadrupole-factorized (Q-factorized) prescription that maps the total energy flux-including horizon absorption-onto a single (2,2) mode baseline. This approach effectively captures higher-order multipole contributions without explicit mode summation, while simultaneously leading to a dramatic reduction in fractional flux errors. To ensure a smooth transition to the post-merger stage, we replace traditional next-to-quasicircular corrections with a phenomenological ansatz, enabling a flexible, mode-dependent attachment prescription. For the merger-ringdown stage, we utilize quasi-normal mode coefficients extracted from numerical waveforms via qnmfinder to explicitly model mode-mixing effects. These enhancements lead to a substantial reduction in residuals, capturing the complex physical modulations prominent in retrograde configurations. Additionally, we implement the (2,0) mode across the full waveform, further extending the model's physical coverage and accuracy. Overall, our framework generates highly accurate late inspiral-merger-ringdown waveforms for extreme-mass-ratio systems, significantly reducing dephasing and improving the near-merger reconstruction. We demonstrate the performance of SEOB-TML against the current state-of-the-art SEOBNRv5HM model, highlighting how our specialized developments extend the reliability of the EOB framework into the test-mass limit.

discussion (0)

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Forward citations

Cited by 3 Pith papers

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    SEOBNRv6EHM is a multipolar EOB model for eccentric planar-orbit BBHs calibrated to NR simulations, showing low waveform mismatches up to eccentricity 0.9.

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Reference graph

Works this paper leans on

192 extracted references · 156 linked inside Pith · cited by 3 Pith papers

  1. [1]

    Because the Newtonian factor for�= 0 is inherently non-circular and vanishes in the circular-orbit limit, factorization can introduce spurious poles and numerical instabilities

    Inspiral modeling As discussed in Ref [185], the standard factorization approach is ill-suited for the m = 0 mode. Because the Newtonian factor for�= 0 is inherently non-circular and vanishes in the circular-orbit limit, factorization can introduce spurious poles and numerical instabilities. Ad- ditionally, it has been demonstrated that keeping all time d...

  2. [2]

    To improve merger–RD accuracy, we attach the merger–RD waveform at the (2�0) peak

    Final stage of inspiral-plunge For the (2�0) mode, particularly in high positive-spin cases, its peak is strongly delayed relative to the (2�2) mode. To improve merger–RD accuracy, we attach the merger–RD waveform at the (2�0) peak. As discussed in Sec. IV, we use a phenomenological hyperbolic ansatz in- stead of the NQC corrections for the last stage of ...

  3. [3]

    [111], we first complex- ify the real (2,0) mode in order to apply the standard merger–RD ansatz used for other modes

    Merger–RD modeling Following the approach in Ref. [111], we first complex- ify the real (2,0) mode in order to apply the standard merger–RD ansatz used for other modes. This is accom- plished by utilizing the Hilbert transform to construct an analytic signal, which provides a well-defined ampli- tude and phase for the otherwise real-valued mode. The Hilbe...

  4. [4]

    Making Sense of the Unexpected in the Gravitational-Wave Sky

    Comparison with Teukolsky waveform We now construct the full IMR (2�0) waveforms and compare them with the TD Teukolsky waveforms. Fig- ure 22 shows the (2�0) mode for spins�=�0�9�0�0�and 0�9, together with the residuals in the bottom panels. The comparison demonstrates that the late-stage IMR signal is accurately modeled overall. However, for large posit...

  5. [5]

    B. P. Abbottet al.(LIGO Scientific, Virgo), GWTC- 1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs, Phys. Rev. X9, 031040 (2019), arXiv:1811.12907 [astro-ph.HE]

    Pith/arXiv arXiv 2019

  6. [6]

    Abbottet al.(LIGO Scientific, Virgo), GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run, Phys

    R. Abbottet al.(LIGO Scientific, Virgo), GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run, Phys. Rev. X11, 021053 (2021), arXiv:2010.14527 [gr- qc]

    Pith/arXiv arXiv 2021

  7. [7]

    R. Abbottet al.(LIGO Scientific, VIRGO), GWTC- 2.1: Deep Extended Catalog of Compact Binary Coales- cences Observed by LIGO and Virgo During the First Half of the Third Observing Run, Phys. Rev. D109, 022001 (2024), arXiv:2108.01045 [gr-qc]

    Pith/arXiv arXiv 2024

  8. [8]

    Abbottet al.(LIGO Scientific, Virgo), Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo, SoftwareX13, 100658 (2021), arXiv:1912.11716 [gr-qc]

    R. Abbottet al.(LIGO Scientific, Virgo), Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo, SoftwareX13, 100658 (2021), arXiv:1912.11716 [gr-qc]

    Pith/arXiv arXiv 2021

  9. [9]

    B. P. Abbottet al.(LIGO Scientific, Virgo), Obser- vation of Gravitational Waves from a Binary Black Hole Merger, Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]

    Pith/arXiv arXiv 2016

  10. [10]

    Abbottet al.(LIGO Scientific, VIRGO, KAGRA), GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run, Phys

    R. Abbottet al.(LIGO Scientific, VIRGO, KAGRA), GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run, Phys. Rev. X13, 041039 (2023), arXiv:2111.03606 [gr-qc]

    Pith/arXiv arXiv 2023

  11. [11]

    B. P. Abbottet al.(KAGRA, LIGO Scientific, Virgo, VIRGO), Prospects for observing and localiz- ing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA, Living Rev. Rel.21, 3 (2018), arXiv:1304.0670 [gr-qc]

    Pith/arXiv arXiv 2018

  12. [12]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), GWTC-4.0: Updating the Gravitational-Wave Tran- sient Catalog with Observations from the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run, (2025), arXiv:2508.18082 [gr-qc]

    Pith/arXiv arXiv 2025

  13. [13]

    Fritschel, S

    P. Fritschel, S. Reid, G. Vajente, G. Hammond, H. Miao, D. Brown, V. Quetschke, and J. Steinlechner, Instrument science white paper 2021, LIGO-T2100298, https://dcc.ligo.org/LIGO-T2100298/public (2021)

    2021

  14. [14]

    T. V. Collaboration, Advanced virgo technical design report, VIR-0128A-12 (2012)

    2012

  15. [15]

    Punturoet al., The einstein telescope: a third- generation gravitational wave observatory, Classical and Quantum Gravity27, 194002 (2010)

    M. Punturoet al., The einstein telescope: a third- generation gravitational wave observatory, Classical and Quantum Gravity27, 194002 (2010)

    2010

  16. [16]

    Maggioreet al.(ET), Science Case for the Ein- stein Telescope, JCAP03, 050, arXiv:1912.02622 [astro- ph.CO]

    M. Maggioreet al.(ET), Science Case for the Ein- stein Telescope, JCAP03, 050, arXiv:1912.02622 [astro- ph.CO]

    Pith/arXiv arXiv 1912

  17. [17]

    Abacet al.(ET), The Science of the Einstein Tele- scope, arXiv:2503.12263 [gr-qc]

    A. Abacet al.(ET), The Science of the Einstein Tele- scope, arXiv:2503.12263 [gr-qc]

    Pith/arXiv arXiv

  18. [18]

    Evanset al., A Horizon Study for Cosmic Ex- plorer: Science, Observatories, and Community, (2021), arXiv:2109.09882 [astro-ph.IM]

    M. Evanset al., A Horizon Study for Cosmic Ex- plorer: Science, Observatories, and Community, (2021), arXiv:2109.09882 [astro-ph.IM]

    Pith/arXiv arXiv 2021

  19. [19]

    Amaro-Seoane, H

    P. Amaro-Seoane, H. Audley, S. Babak, J. Baker, E. Ba- rausse, P. Bender, E. Berti, P. Binetruy, M. Born, D. Bortoluzzi,et al.(LISA), Laser Interferometer Space Antenna, arXiv:1702.00786 [astro-ph.IM]

    Pith/arXiv arXiv

  20. [20]

    Colpiet al.(LISA), LISA Definition Study Report, arXiv:2402.07571 [astro-ph.CO]

    M. Colpiet al.(LISA), LISA Definition Study Report, arXiv:2402.07571 [astro-ph.CO]

    Pith/arXiv arXiv

  21. [21]

    Pretorius, Evolution of binary black hole space- times, Phys

    F. Pretorius, Evolution of binary black hole space- times, Phys. Rev. Lett.95, 121101 (2005), arXiv:gr- qc/0507014

    arXiv 2005

  22. [22]

    Campanelli, C

    M. Campanelli, C. O. Lousto, P. Marronetti, and Y. Zlo- chower, Accurate evolutions of orbiting black-hole bi- naries without excision, Phys. Rev. Lett.96, 111101 (2006), arXiv:gr-qc/0511048

    Pith/arXiv arXiv 2006

  23. [23]

    J. G. Baker, J. Centrella, D.-I. Choi, M. Koppitz, and J. van Meter, Gravitational wave extraction from an inspiraling configuration of merging black holes, Phys. Rev. Lett.96, 111102 (2006), arXiv:gr-qc/0511103

    Pith/arXiv arXiv 2006

  24. [24]

    Blackman, S

    J. Blackman, S. E. Field, C. R. Galley, B. Szil´ agyi, M. A. Scheel, M. Tiglio, and D. A. Hemberger, Fast and Accurate Prediction of Numerical Relativity Wave- forms from Binary Black Hole Coalescences Using Sur- rogate Models, Phys. Rev. Lett.115, 121102 (2015), arXiv:1502.07758 [gr-qc]

    Pith/arXiv arXiv 2015

  25. [25]

    Blackman, S

    J. Blackman, S. E. Field, M. A. Scheel, C. R. Gal- ley, D. A. Hemberger, P. Schmidt, and R. Smith, A Surrogate Model of Gravitational Waveforms from Numerical Relativity Simulations of Precessing Binary Black Hole Mergers, Phys. Rev. D95, 104023 (2017), arXiv:1701.00550 [gr-qc]

    Pith/arXiv arXiv 2017

  26. [26]

    Blackman, S

    J. Blackman, S. E. Field, M. A. Scheel, C. R. Galley, C. D. Ott, M. Boyle, L. E. Kidder, H. P. Pfeiffer, and B. Szil´ agyi, Numerical relativity waveform surrogate model for generically precessing binary black hole merg- ers, Phys. Rev. D96, 024058 (2017), arXiv:1705.07089 [gr-qc]

    Pith/arXiv arXiv 2017

  27. [27]

    Varma, S

    V. Varma, S. E. Field, M. A. Scheel, J. Black- man, L. E. Kidder, and H. P. Pfeiffer, Surrogate model of hybridized numerical relativity binary black hole waveforms, Phys. Rev. D99, 064045 (2019), arXiv:1812.07865 [gr-qc]

    Pith/arXiv arXiv 2019

  28. [28]

    Varma, S

    V. Varma, S. E. Field, M. A. Scheel, J. Blackman, D. Gerosa, L. C. Stein, L. E. Kidder, and H. P. Pfeiffer, Surrogate models for precessing binary black hole sim- ulations with unequal masses, Phys. Rev. Research.1, 033015 (2019), arXiv:1905.09300 [gr-qc]

    Pith/arXiv arXiv 2019

  29. [29]

    Williams, I

    D. Williams, I. S. Heng, J. Gair, J. A. Clark, and B. Khamesra, Precessing numerical relativity waveform surrogate model for binary black holes: A Gaussian process regression approach, Phys. Rev. D101, 063011 (2020), arXiv:1903.09204 [gr-qc]

    Pith/arXiv arXiv 2020

  30. [30]

    N. E. M. Rifat, S. E. Field, G. Khanna, and V. Varma, Surrogate model for gravitational wave signals from comparable and large-mass-ratio black hole binaries, Phys. Rev. D101, 081502 (2020), arXiv:1910.10473 [gr- qc]

    Pith/arXiv arXiv 2020

  31. [31]

    Islam, V

    T. Islam, V. Varma, J. Lodman, S. E. Field, G. Khanna, M. A. Scheel, H. P. Pfeiffer, D. Gerosa, and L. E. Kid- der, Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: compa- rable mass, nonspinning case, Phys. Rev. D103, 064022 (2021), arXiv:2101.11798 [gr-qc]

    Pith/arXiv arXiv 2021

  32. [32]

    Islam, S

    T. Islam, S. E. Field, S. A. Hughes, G. Khanna, V. Varma, M. Giesler, M. A. Scheel, L. E. Kidder, and H. P. Pfeiffer, Surrogate model for gravitational wave signals from nonspinning, comparable-to large- mass-ratio black hole binaries built on black hole pertur- bation theory waveforms calibrated to numerical relativ- 34 ity, Phys. Rev. D106, 104025 (2022...

    Pith/arXiv arXiv 2022

  33. [33]

    J. Yoo, V. Varma, M. Giesler, M. A. Scheel, C.-J. Haster, H. P. Pfeiffer, L. E. Kidder, and M. Boyle, Targeted large mass ratio numerical relativity surro- gate waveform model for GW190814, Phys. Rev. D106, 044001 (2022), arXiv:2203.10109 [gr-qc]

    Pith/arXiv arXiv 2022

  34. [34]

    Islam, G

    T. Islam, G. Khanna, and S. E. Field, Adding higher- order spherical harmonics in nonspinning eccentric bi- nary black hole merger waveform models, Phys. Rev. D 111, 124023 (2025), arXiv:2408.02762 [gr-qc]

    Pith/arXiv arXiv 2025

  35. [35]

    K. Rink, R. Bachhar, T. Islam, N. E. M. Rifat, K. Gonzalez-Quesada, S. E. Field, G. Khanna, S. A. Hughes, and V. Varma, Gravitational wave surrogate model for spinning, intermediate mass ratio binaries based on perturbation theory and numerical relativity, Phys. Rev. D110, 124069 (2024), arXiv:2407.18319 [gr- qc]

    Pith/arXiv arXiv 2024

  36. [36]

    Maurya, P

    A. Maurya, P. Kumar, S. E. Field, C. K. Mishra, P. J. Nee, K. Paul, H. P. Pfeiffer, A. Ravichandran, and V. Varma, Chase Orbits, not Time: A Scalable Paradigm for Long-Duration Eccentric Gravitational- Wave Surrogates, arXiv:2510.00116 [gr-qc]

    arXiv

  37. [37]

    P. J. Neeet al., Eccentric binary black holes: A new framework for numerical relativity waveform surrogates, (2025), arXiv:2510.00106 [gr-qc]

    arXiv 2025

  38. [38]

    Y. Pan, A. Buonanno, J. G. Baker, J. Centrella, B. J. Kelly, S. T. McWilliams, F. Pretorius, and J. R. van Me- ter, A Data-analysis driven comparison of analytic and numerical coalescing binary waveforms: Nonspinning case, Phys. Rev. D77, 024014 (2008), arXiv:0704.1964 [gr-qc]

    Pith/arXiv arXiv 2008

  39. [39]

    Ajithet al., Phenomenological template family for black-hole coalescence waveforms, Class

    P. Ajithet al., Phenomenological template family for black-hole coalescence waveforms, Class. Quant. Grav. 24, S689 (2007), arXiv:0704.3764 [gr-qc]

    Pith/arXiv arXiv 2007

  40. [40]

    Ajithet al., Inspiral-merger-ringdown waveforms for black-hole binaries with non-precessing spins, Phys

    P. Ajithet al., Inspiral-merger-ringdown waveforms for black-hole binaries with non-precessing spins, Phys. Rev. Lett.106, 241101 (2011), arXiv:0909.2867 [gr-qc]

    Pith/arXiv arXiv 2011

  41. [41]

    Santamariaet al., Matching post-Newtonian and numerical relativity waveforms: systematic errors and a new phenomenological model for non-precessing black hole binaries, Phys

    L. Santamariaet al., Matching post-Newtonian and numerical relativity waveforms: systematic errors and a new phenomenological model for non-precessing black hole binaries, Phys. Rev. D82, 064016 (2010), arXiv:1005.3306 [gr-qc]

    Pith/arXiv arXiv 2010

  42. [42]

    Hannam, P

    M. Hannam, P. Schmidt, A. Boh´ e, L. Haegel, S. Husa, F. Ohme, G. Pratten, and M. P¨ urrer, Simple Model of Complete Precessing Black-Hole-Binary Gravita- tional Waveforms, Phys. Rev. Lett.113, 151101 (2014), arXiv:1308.3271 [gr-qc]

    Pith/arXiv arXiv 2014

  43. [43]

    S. Husa, S. Khan, M. Hannam, M. P¨ urrer, F. Ohme, X. Jim´ enez Forteza, and A. Boh´ e, Frequency-domain gravitational waves from nonprecessing black-hole bi- naries. I. New numerical waveforms and anatomy of the signal, Phys. Rev. D93, 044006 (2016), arXiv:1508.07250 [gr-qc]

    Pith/arXiv arXiv 2016

  44. [44]

    S. Khan, S. Husa, M. Hannam, F. Ohme, M. P¨ urrer, X. Jim´ enez Forteza, and A. Boh´ e, Frequency-domain gravitational waves from nonprecessing black-hole bi- naries. II. A phenomenological model for the ad- vanced detector era, Phys. Rev. D93, 044007 (2016), arXiv:1508.07253 [gr-qc]

    Pith/arXiv arXiv 2016

  45. [45]

    London, S

    L. London, S. Khan, E. Fauchon-Jones, C. Garc´ ıa, M. Hannam, S. Husa, X. Jim´ enez-Forteza, C. Kalaghatgi, F. Ohme, and F. Pannarale, First higher-multipole model of gravitational waves from spinning and coalescing black-hole binaries, Phys. Rev. Lett.120, 161102 (2018), arXiv:1708.00404 [gr-qc]

    Pith/arXiv arXiv 2018

  46. [46]

    S. Khan, K. Chatziioannou, M. Hannam, and F. Ohme, Phenomenological model for the gravitational-wave sig- nal from precessing binary black holes with two- spin effects, Phys. Rev. D100, 024059 (2019), arXiv:1809.10113 [gr-qc]

    Pith/arXiv arXiv 2019

  47. [47]

    S. Khan, F. Ohme, K. Chatziioannou, and M. Hannam, Including higher order multipoles in gravitational-wave models for precessing binary black holes, Phys. Rev. D 101, 024056 (2020), arXiv:1911.06050 [gr-qc]

    Pith/arXiv arXiv 2020

  48. [48]

    Pratten, S

    G. Pratten, S. Husa, C. Garcia-Quiros, M. Colleoni, A. Ramos-Buades, H. Estelles, and R. Jaume, Setting the cornerstone for a family of models for gravitational waves from compact binaries: The dominant harmonic for nonprecessing quasicircular black holes, Phys. Rev. D102, 064001 (2020), arXiv:2001.11412 [gr-qc]

    Pith/arXiv arXiv 2020

  49. [49]

    Prattenet al., Computationally efficient models for the dominant and subdominant harmonic modes of pre- cessing binary black holes, Phys

    G. Prattenet al., Computationally efficient models for the dominant and subdominant harmonic modes of pre- cessing binary black holes, Phys. Rev. D103, 104056 (2021), arXiv:2004.06503 [gr-qc]

    Pith/arXiv arXiv 2021

  50. [50]

    Garc´ ıa-Quir´ os, M

    C. Garc´ ıa-Quir´ os, M. Colleoni, S. Husa, H. Estell´ es, G. Pratten, A. Ramos-Buades, M. Mateu-Lucena, and R. Jaume, Multimode frequency-domain model for the gravitational wave signal from nonprecessing black-hole binaries, Phys. Rev. D102, 064002 (2020), arXiv:2001.10914 [gr-qc]

    Pith/arXiv arXiv 2020

  51. [51]

    Hamilton, L

    E. Hamilton, L. London, J. E. Thompson, E. Fauchon- Jones, M. Hannam, C. Kalaghatgi, S. Khan, F. Pannar- ale, and A. Vano-Vinuales, Model of gravitational waves from precessing black-hole binaries through merger and ringdown, Phys. Rev. D104, 124027 (2021), arXiv:2107.08876 [gr-qc]

    Pith/arXiv arXiv 2021

  52. [52]

    J. E. Thompson, E. Hamilton, L. London, S. Ghosh, P. Kolitsidou, C. Hoy, and M. Hannam, PhenomXO4a: a phenomenological gravitational-wave model for pre- cessing black-hole binaries with higher multipoles and asymmetries, Phys. Rev. D109, 063012 (2024), arXiv:2312.10025 [gr-qc]

    Pith/arXiv arXiv 2024

  53. [53]

    Colleoni, F

    M. Colleoni, F. A. R. Vidal, C. Garc´ ıa-Quir´ os, S. Ak¸ cay, and S. Bera, Fast frequency-domain gravitational wave- forms for precessing binaries with a new twist, Phys. Rev. D111, 104019 (2025), arXiv:2412.16721 [gr-qc]

    Pith/arXiv arXiv 2025

  54. [54]

    Hamiltonet al., PhenomXPNR: An improved grav- itational wave model linking precessing inspirals and NR-calibrated merger-ringdown, arXiv:2507.02604 [gr- qc]

    E. Hamiltonet al., PhenomXPNR: An improved grav- itational wave model linking precessing inspirals and NR-calibrated merger-ringdown, arXiv:2507.02604 [gr- qc]

    Pith/arXiv arXiv

  55. [55]

    Ramos-Buades, Q

    A. Ramos-Buades, Q. Henry, and M. Haney, Fast frequency-domain phenomenological modeling of eccen- tric aligned-spin binary black holes, arXiv:2601.03340 [gr-qc]

    arXiv

  56. [56]

    Estell´ es, S

    H. Estell´ es, S. Husa, M. Colleoni, D. Keitel, M. Mateu- Lucena, C. Garc´ ıa-Quir´ os, A. Ramos-Buades, and A. Borchers, Time-domain phenomenological model of gravitational-wave subdominant harmonics for quasi- circular nonprecessing binary black hole coalescences, Phys. Rev. D105, 084039 (2022), arXiv:2012.11923 [gr- qc]

    Pith/arXiv arXiv 2022

  57. [57]

    Estell´ es, A

    H. Estell´ es, A. Ramos-Buades, S. Husa, C. Garc´ ıa- Quir´ os, M. Colleoni, L. Haegel, and R. Jaume, Phenomenological time domain model for dominant quadrupole gravitational wave signal of coalescing bi- nary black holes, Phys. Rev. D103, 124060 (2021), arXiv:2004.08302 [gr-qc]. 35

    Pith/arXiv arXiv 2021

  58. [58]

    Estell´ es, M

    H. Estell´ es, M. Colleoni, C. Garc´ ıa-Quir´ os, S. Husa, D. Keitel, M. Mateu-Lucena, M. d. L. Planas, and A. Ramos-Buades, New twists in compact bi- nary waveform modeling: A fast time-domain model for precession, Phys. Rev. D105, 084040 (2022), arXiv:2105.05872 [gr-qc]

    Pith/arXiv arXiv 2022

  59. [59]

    Rossell´ o-Sastre, S

    M. Rossell´ o-Sastre, S. Husa, and S. Bera, Waveform model for the missing quadrupole mode from black hole coalescence: Memory effect and ringdown of the (ℓ=2,m=0) spherical harmonic, Phys. Rev. D110, 084074 (2024), arXiv:2405.17302 [gr-qc]

    Pith/arXiv arXiv 2024

  60. [60]

    M. d. L. Planas, A. Ramos-Buades, C. Garc´ ıa-Quir´ os, H. Estell´ es, S. Husa, and M. Haney, Time-domain phe- nomenological multipolar waveforms for aligned-spin bi- nary black holes in elliptical orbits, Phys. Rev. D113, 024006 (2026), arXiv:2503.13062 [gr-qc]

    arXiv 2026

  61. [61]

    Buonanno and T

    A. Buonanno and T. Damour, Effective one-body ap- proach to general relativistic two-body dynamics, Phys. Rev. D59, 084006 (1999), arXiv:gr-qc/9811091

    Pith/arXiv arXiv 1999

  62. [62]

    Buonanno and T

    A. Buonanno and T. Damour, Transition from inspiral to plunge in binary black hole coalescences, Phys. Rev. D62, 064015 (2000), arXiv:gr-qc/0001013

    Pith/arXiv arXiv 2000

  63. [63]

    Damour, P

    T. Damour, P. Jaranowski, and G. Schaefer, On the determination of the last stable orbit for circular gen- eral relativistic binaries at the third postNewtonian ap- proximation, Phys. Rev. D62, 084011 (2000), arXiv:gr- qc/0005034

    arXiv 2000

  64. [64]

    Damour, Coalescence of two spinning black holes: an effective one-body approach, Phys

    T. Damour, Coalescence of two spinning black holes: an effective one-body approach, Phys. Rev. D64, 124013 (2001), arXiv:gr-qc/0103018

    Pith/arXiv arXiv 2001

  65. [65]

    Buonanno, Y

    A. Buonanno, Y. Chen, and T. Damour, Transition from inspiral to plunge in precessing binaries of spinning black holes, Phys. Rev. D74, 104005 (2006), arXiv:gr- qc/0508067

    arXiv 2006

  66. [66]

    Buonanno, G

    A. Buonanno, G. B. Cook, and F. Pretorius, Inspiral, merger and ring-down of equal-mass black-hole binaries, Phys. Rev. D75, 124018 (2007), arXiv:gr-qc/0610122

    Pith/arXiv arXiv 2007

  67. [67]

    Buonanno, Y

    A. Buonanno, Y. Pan, J. G. Baker, J. Centrella, B. J. Kelly, S. T. McWilliams, and J. R. van Meter, Toward faithful templates for non-spinning binary black holes using the effective-one-body approach, Phys. Rev. D76, 104049 (2007), arXiv:0706.3732 [gr-qc]

    Pith/arXiv arXiv 2007

  68. [68]

    Buonanno, Y

    A. Buonanno, Y. Pan, H. P. Pfeiffer, M. A. Scheel, L. T. Buchman, and L. E. Kidder, Effective-one-body waveforms calibrated to numerical relativity simula- tions: Coalescence of non-spinning, equal-mass black holes, Phys. Rev. D79, 124028 (2009), arXiv:0902.0790 [gr-qc]

    Pith/arXiv arXiv 2009

  69. [69]

    Y. Pan, A. Buonanno, M. Boyle, L. T. Buchman, L. E. Kidder, H. P. Pfeiffer, and M. A. Scheel, Inspiral- merger-ringdown multipolar waveforms of nonspinning black-hole binaries using the effective-one-body formal- ism, Phys. Rev. D84, 124052 (2011), arXiv:1106.1021 [gr-qc]

    Pith/arXiv arXiv 2011

  70. [70]

    Damour, A

    T. Damour, A. Nagar, and S. Bernuzzi, Improved effective-one-body description of coalescing nonspinning black-hole binaries and its numerical-relativity comple- tion, Phys. Rev. D87, 084035 (2013), arXiv:1212.4357 [gr-qc]

    Pith/arXiv arXiv 2013

  71. [71]

    Damour, P

    T. Damour, P. Jaranowski, and G. Sch¨ afer, Fourth post- Newtonian effective one-body dynamics, Phys. Rev. D 91, 084024 (2015), arXiv:1502.07245 [gr-qc]

    Pith/arXiv arXiv 2015

  72. [72]

    Y. Pan, A. Buonanno, L. T. Buchman, T. Chu, L. E. Kidder, H. P. Pfeiffer, and M. A. Scheel, Effective-one- body waveforms calibrated to numerical relativity simu- lations: coalescence of non-precessing, spinning, equal- mass black holes, Phys. Rev. D81, 084041 (2010), arXiv:0912.3466 [gr-qc]

    Pith/arXiv arXiv 2010

  73. [73]

    Taracchini, Y

    A. Taracchini, Y. Pan, A. Buonanno, E. Barausse, M. Boyle, T. Chu, G. Lovelace, H. P. Pfeiffer, and M. A. Scheel, Prototype effective-one-body model for nonprecessing spinning inspiral-merger-ringdown wave- forms, Phys. Rev. D86, 024011 (2012), arXiv:1202.0790 [gr-qc]

    Pith/arXiv arXiv 2012

  74. [74]

    Taracchiniet al., Effective-one-body model for black- hole binaries with generic mass ratios and spins, Phys

    A. Taracchiniet al., Effective-one-body model for black- hole binaries with generic mass ratios and spins, Phys. Rev. D89, 061502 (2014), arXiv:1311.2544 [gr-qc]

    Pith/arXiv arXiv 2014

  75. [75]

    Boh´ eet al., Improved effective-one-body model of spinning, nonprecessing binary black holes for the era of gravitational-wave astrophysics with advanced detec- tors, Phys

    A. Boh´ eet al., Improved effective-one-body model of spinning, nonprecessing binary black holes for the era of gravitational-wave astrophysics with advanced detec- tors, Phys. Rev. D95, 044028 (2017), arXiv:1611.03703 [gr-qc]

    Pith/arXiv arXiv 2017

  76. [76]

    Cotesta, A

    R. Cotesta, A. Buonanno, A. Boh´ e, A. Taracchini, I. Hinder, and S. Ossokine, Enriching the Symphony of Gravitational Waves from Binary Black Holes by Tun- ing Higher Harmonics, Phys. Rev. D98, 084028 (2018), arXiv:1803.10701 [gr-qc]

    Pith/arXiv arXiv 2018

  77. [77]

    Ossokineet al., Multipolar Effective-One-Body Wave- forms for Precessing Binary Black Holes: Construc- tion and Validation, Phys

    S. Ossokineet al., Multipolar Effective-One-Body Wave- forms for Precessing Binary Black Holes: Construc- tion and Validation, Phys. Rev. D102, 044055 (2020), arXiv:2004.09442 [gr-qc]

    Pith/arXiv arXiv 2020

  78. [78]

    Pompili, A

    L. Pompili, A. Buonanno, H. Estell´ es, M. Khalil, M. van de Meent, D. Mihaylov, S. Ossokine, M. P¨ urrer, A. Ramos-Buades,et al., Laying the foundation of the effective-one-body waveform models SEOBNRv5: Im- proved accuracy and efficiency for spinning nonprecess- ing binary black holes, Phys. Rev. D108, 124035 (2023), arXiv:2303.18039 [gr-qc]

    Pith/arXiv arXiv 2023

  79. [79]

    Ramos-Buades, A

    A. Ramos-Buades, A. Buonanno, H. Estell´ es, M. Khalil, D. P. Mihaylov, S. Ossokine, L. Pompili, and M. Shiferaw, Next generation of accurate and ef- ficient multipolar precessing-spin effective-one-body waveforms for binary black holes, Phys. Rev. D108, 124037 (2023), arXiv:2303.18046 [gr-qc]

    Pith/arXiv arXiv 2023

  80. [80]

    Gamboa, M

    A. Gamboa, M. Khalil, and A. Buonanno, Third post-Newtonian dynamics for eccentric orbits and aligned spins in the effective-one-body waveform model seobnrv5ehm, Phys. Rev. D112, 044037 (2025), arXiv:2412.12831 [gr-qc]

    Pith/arXiv arXiv 2025

Showing first 80 references.