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arxiv: 2605.28716 · v1 · pith:5O3M4R3Wnew · submitted 2026-05-27 · 🌀 gr-qc

Eccentric and unbound compact binaries in the LIGO-Virgo-KAGRA catalog: parameter estimation and waveform systematics with SEOBNRv6EHM

Lorenzo Pompili , Aldo Gamboa , Alessandra Buonanno This is my paper

Pith reviewed 2026-06-29 10:33 UTC · model grok-4.3

classification 🌀 gr-qc
keywords eccentric binariesgravitational wave parameter estimationSEOBNR waveformsLIGO-Virgo-KAGRA catalogbinary black holesunbound orbitsBayes factors
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The pith

SEOBNRv6EHM reduces biases in eccentricity, masses, and spins for gravitational-wave signals from eccentric binaries and shows mild support for eccentricity in five catalog events.

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

The paper tests the SEOBNRv6EHM waveform model on synthetic signals from long, highly eccentric numerical-relativity simulations and finds that it recovers eccentricity, masses, and spins with less bias than SEOBNRv5EHM or TEOBResumS-Dalí. It then applies the model to 26 events from the LIGO-Virgo-KAGRA catalog. Five events show log10 Bayes factors greater than 0.5 favoring eccentric aligned-spin over quasi-circular precessing-spin hypotheses. For five high-mass events the model also permits unbound initial conditions, yielding marginal support in three cases including GW190521.

Core claim

SEOBNRv6EHM significantly reduces biases in eccentricity, masses, and spins relative to earlier eccentric models; five events have log10 B_EAS_QCP > 0.5 and three high-mass events including GW190521 have log10 B_unbound_QCP approximately 0.2 to 0.6, though the recovered unbound configurations remain astrophysically unrealistic and cannot be confidently separated from highly eccentric bound orbits.

What carries the argument

The SEOBNRv6EHM effective-one-body waveform model for generic planar binaries, which enables parameter estimation with eccentricity and unbound initial conditions.

Load-bearing premise

The long, highly eccentric numerical-relativity waveforms used as synthetic signals represent the relevant parameter space and any remaining model error does not systematically affect the Bayes-factor comparisons.

What would settle it

Recovery of the same synthetic signals with SEOBNRv6EHM producing eccentricity or mass biases comparable to those from SEOBNRv5EHM would falsify the reduction in bias.

Figures

Figures reproduced from arXiv: 2605.28716 by Aldo Gamboa, Alessandra Buonanno, Lorenzo Pompili.

Figure 1
Figure 1. Figure 1: Whitened-strain waveforms in the LIGO Hanford de [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Instantaneous and orbit-averaged frequency of the (2 [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Reconstruction of the gravitational-wave eccentricity [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Posterior distributions of GW eccentricity [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Whitened-strain waveform reconstruction for the highest-eccentricity NR configuration ( [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Wall-clock run times for the four benchmark events ana [PITH_FULL_IMAGE:figures/full_fig_p014_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: log10 Bayes factor favoring the eccentric aligned-spin (EAS) hypothesis over the quasi-circular aligned-spin (QCAS) hypothesis as a function of the median posterior eccentricity e at the orbit-averaged starting frequency ⟨fstart⟩ for the 26 gravitational-wave events analyzed with SEOBNRv6EHM. Crosshairs indicate the 90% credible intervals on the eccentricity (horizontal) and the Bayes factor (vertical). Th… view at source ↗
Figure 8
Figure 8. Figure 8: Comparison of the log10 Bayes factor favoring the eccentric aligned-spin (EAS) hypothesis over the quasi-circular aligned-spin (QCAS) hypothesis (filled markers) against the Bayes factor favoring EAS over the quasi-circular precessing-spin (QCP) hypothesis (open markers), for the six events in Table IV with log10 B EAS QCAS > 0.5. port reported with IMRPhenomTEHM [100] and TEOBResumS￾Dal´ı [93, 101]. This … view at source ↗
Figure 9
Figure 9. Figure 9: Posterior distributions of eccentricity e and relativistic anomaly ζ at the orbit-averaged starting frequency of waveform generation (⟨fstart⟩ = 20 Hz for GW200105 162426 and 10 Hz for all other events), for the six events with the highest Bayes factor favoring eccentricity. Contours show the 50% and 90% credible regions. The eccentricity axis starts at e = 0 for all events except GW200129 065458, whose po… view at source ↗
Figure 10
Figure 10. Figure 10: Marginal posteriors on the detector-frame total mass [PITH_FULL_IMAGE:figures/full_fig_p021_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Log Bayes factors log10 B unbound EAS (filled markers) and log10 B unbound QCP comparing the unbound hypothesis against the bound eccentric aligned-spin (EAS) and quasi-circular precessing-spin (QCP) hypotheses, respectively, for the five high-mass events analyzed under unbound initial conditions. The QCP markers are shown for two precessing waveform models: SEOBNRv5PHM (open markers) and NRSur7dq4 (half￾… view at source ↗
Figure 12
Figure 12. Figure 12: Analysis of GW190521, GW191109 010717, and GW231221 135041 under the unbound-orbit hypothesis with SEOBNRv6EHM. For each event: Left: Whitened waveform reconstruction in the LIGO Hanford (top) and Livingston (bottom) detectors. The median (solid) and 90% credible interval (shaded) of the reconstructed distribution are shown for the unbound SEOBNRv6EHM model and the quasi-circular precessing-spin model NRS… view at source ↗
Figure 13
Figure 13. Figure 13: Impact of the waveform starting frequency on recovered parameters for three NR injection configurations: [PITH_FULL_IMAGE:figures/full_fig_p027_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Whitened-strain waveform reconstruction in the LIGO Hanford detector for the [PITH_FULL_IMAGE:figures/full_fig_p028_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Median waveform evaluation time for SEOBNRv5EHM, SEOBNRv6EHM, and TEOBResumS-Dal´ı for the four benchmark events. For each event, 100 parameter samples are drawn from the SEOBNRv6EHM posterior and used to evaluate waveforms with each model under identical settings. Each group of bars corre￾sponds to one event, with the signal duration and binary type indi￾cated below. Time labels are shown above each bar.… view at source ↗
Figure 16
Figure 16. Figure 16: Posterior samples for GW200105 162426 in the standard polar eccentricity parameterization (left, e vs ζ) and the Cartesian parameterization (right, ex vs ey), colored by the log-likelihood value. In polar coordinates, the anomaly is unconstrained across [0, 2π] at each eccentricity value. dial marginal p(e) = 1/emax is uniform by construction. The waveform generator converts (ex, ey) back to (e, ζ) before… view at source ↗
Figure 17
Figure 17. Figure 17: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p031_17.png] view at source ↗
read the original abstract

Orbital eccentricity encodes key information about compact-binary formation channels and astrophysical environments, making it a critical target for gravitational-wave (GW) inference. We present parameter-estimation (PE) analyses of GWs from eccentric compact binaries with the SEOBNRv6EHM waveform model. Using long, highly eccentric numerical-relativity waveforms as synthetic signals, we compare parameter recovery across state-of-the-art eccentric models. We find that SEOBNRv5EHM and TEOBResumS-Dal\'i can yield biased estimates of eccentricity, masses, and spins in the most challenging configurations, while SEOBNRv6EHM significantly reduces these biases. Applying SEOBNRv6EHM to 26 GW events from the O1--O4 LIGO--Virgo--KAGRA observing runs -- including binary black hole, neutron-star--black-hole, and binary neutron-star mergers -- we identify five events with mild support for eccentricity over the quasi-circular precessing-spin hypothesis, with Bayes factors $\log_{10} \mathcal{B}^{\text{EAS}}_{\text{QCP}} > 0.5$. Since SEOBNRv6EHM is applicable to generic planar binaries, we reanalyze five high-mass events allowing for unbound initial conditions. For three of them -- including GW190521, previously claimed to originate from a dynamical capture -- a direct-capture configuration is comparable to, or marginally favored over, both the eccentric aligned-spin and quasi-circular precessing-spin hypotheses ($\log_{10}\mathcal{B}^{\rm unbound}_{\rm QCP} \approx 0.2$--$0.6$ for GW190521). The recovered configurations are, however, astrophysically unrealistic and cannot be confidently discriminated from highly eccentric bound orbits, so these results do not, by themselves, support an unbound origin for these events. SEOBNRv6EHM is approximately three times faster in PE analyses than SEOBNRv5EHM, while improving waveform accuracy, enabling efficient, large-scale GW inference with eccentric waveforms.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

0 major / 1 minor

Summary. The manuscript introduces the SEOBNRv6EHM waveform model for eccentric and unbound compact binaries. Using long, highly eccentric numerical-relativity waveforms as synthetic signals, it demonstrates that SEOBNRv6EHM reduces biases in recovered eccentricity, masses, and spins relative to SEOBNRv5EHM and TEOBResumS-Dalí. The model is applied to 26 events from the O1–O4 LIGO-Virgo-KAGRA catalog, identifying five events with mild support for eccentricity (log10 B_EAS_QCP > 0.5) and three high-mass events (including GW190521) with mild support for unbound initial conditions (log10 B_unbound_QCP ≈ 0.2–0.6), while explicitly noting that recovered unbound configurations are astrophysically unrealistic and cannot be confidently distinguished from highly eccentric bound orbits. The model is also reported to be approximately three times faster than SEOBNRv5EHM in parameter estimation.

Significance. If the reported bias reductions hold under the full set of tests, the work provides a practically useful improvement in eccentric waveform modeling that supports more reliable eccentricity measurements from gravitational-wave data, which is directly relevant to formation-channel studies. The speed improvement and the systematic application to the catalog (with built-in caveats on the mild Bayes factors) strengthen the contribution for enabling larger-scale analyses.

minor comments (1)
  1. [Abstract] Abstract: the claim that SEOBNRv6EHM is 'approximately three times faster in PE analyses' should include a specific cross-reference to the timing benchmarks or table in the methods or results sections.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of our manuscript, the recognition of SEOBNRv6EHM's improvements in reducing parameter biases for eccentric binaries, the speed gains, and the appropriate caveats on the mild Bayes factors. We appreciate the recommendation for minor revision.

Circularity Check

0 steps flagged

No significant circularity identified

full rationale

The paper validates SEOBNRv6EHM by injecting independent long highly eccentric NR waveforms and recovering parameters, then applies the model to real catalog events to compute Bayes factors. No equations or central claims reduce by construction to fitted inputs from the same data, self-definitional loops, or load-bearing self-citations whose validity depends on the present work. The reported bias reductions and mild log10 B values are externally falsifiable against NR and catalog data, with explicit caveats on astrophysical interpretation, rendering the derivation chain self-contained.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Only the abstract is available, so the full set of free parameters, axioms, and invented entities cannot be audited. The model is an incremental update to the established SEOBNR effective-one-body framework; any new eccentric or unbound terms are not enumerated here.

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Forward citations

Cited by 4 Pith papers

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

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