pith. sign in

arxiv: 2606.28156 · v1 · pith:CSID4STInew · submitted 2026-06-26 · 🌀 gr-qc · astro-ph.HE

Joint inference of line-of-sight acceleration and orbital eccentricity in neutron-star--black-hole binaries

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

Pith reviewed 2026-06-29 03:21 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.HE
keywords gravitational wavesline-of-sight accelerationorbital eccentricityneutron-star black-hole binarieswaveform modelingLIGO-Virgo-KAGRA eventsdynamical formation
0
0 comments X

The pith

All five neutron-star black-hole mergers remain consistent with zero line-of-sight acceleration.

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

The paper develops a time-domain remapping of gravitational-wave strain that adds the Doppler shift from line-of-sight acceleration uniformly to any waveform content. This correction is implemented inside both an eccentric aligned-spin model and a precessing quasi-circular model. Validation on simulated signals shows the eccentric model recovers injected acceleration correctly while the precessing model produces spurious signals on eccentric injections. The method is then used for the first joint inference of acceleration and eccentricity on the five neutron-star black-hole events in the catalog. All five events are found consistent with vanishing acceleration, though the joint posterior for one event still disfavors both acceleration and eccentricity being zero at 90 percent credibility.

Core claim

Implementing line-of-sight acceleration as a direct time-domain remap of the strain inside SEOBNRv6EHM recovers the acceleration parameter correctly on both eccentric and spin-precessing injections, whereas SEOBNRv5PHM yields spurious acceleration measurements on eccentric signals. When the same framework is applied to the five NSBH events, every event is consistent with Γ ≡ a∥/c = 0; the joint (Γ, e) posterior for GW200105_162426 nevertheless disfavors the case in which both parameters are simultaneously zero at 90 percent credibility.

What carries the argument

The time-domain remapping of the strain that incorporates the Doppler modulation from line-of-sight acceleration, which applies uniformly across all modes, precession, and eccentricity.

If this is right

  • The eccentric waveform model can be trusted for LOSA measurements even when orbital eccentricity is present.
  • Three NSBH events receive their first published LOSA constraints.
  • Joint inference of LOSA and eccentricity supplies a single-event diagnostic for dynamical formation channels.
  • Previous eccentricity hints in GW200105_162426 survive after marginalizing over possible line-of-sight acceleration.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Future higher-accuracy waveforms could decide whether the remaining tension in GW200105 reflects a genuine dynamical signature or residual model error.
  • Extending the same joint analysis to additional compact-binary classes might reveal statistical patterns linking acceleration to specific tertiary perturbers.
  • The uniform treatment of eccentricity and acceleration reduces the chance that one effect is misattributed to the other in upcoming detections.

Load-bearing premise

The chosen SEOBNR waveform models together with the LOSA remapping fully capture all relevant physics and do not introduce unmodeled systematics that could mimic or mask a true LOSA signal.

What would settle it

A future NSBH event whose joint posterior strongly favors non-zero LOSA at high credibility, or an injection-recovery test in which the remapping fails to recover a known injected acceleration once additional physical effects are included.

Figures

Figures reproduced from arXiv: 2606.28156 by Aldo Gamboa, Alessandra Buonanno, Lorenzo Pompili.

Figure 1
Figure 1. Figure 1: Illustration of a constant LOSA Γ ≡ a∥/c on the plus po￾larization h+(t) of a time-domain waveform, aligned at the merger (t = 0) and shown over a short time window. The reference (Γ = 0) waveform is compared with Γ > 0 and Γ < 0, for a non-spinning bi￾nary with chirp mass M = 6.5 M⊙, mass ratio q = 2, and eccentricity e = 0.30 at ⟨fref⟩ = 20 Hz, generated with SEOBNRv6EHM. We take |Γ| = 10−1 s −1 , well a… view at source ↗
Figure 2
Figure 2. Figure 2: Mismatch 1 − O (with O the noise-weighted over￾lap between two waveforms, maximized over time and phase) be￾tween the time-domain LOSA implementation in SEOBNRv6EHM and the frequency-domain one in Bilby TGR [64, 74] applied to IMRPhenomXAS, as a function of the LOSA parameter Γ and detector￾frame chirp mass M. Overlaps are computed against the A+ de￾sign PSD for non-spinning quasi-circular binaries with q … view at source ↗
Figure 4
Figure 4. Figure 4: Validation on the quasi-circular precessing (QCP) (left) and eccentric aligned-spin (EAS) (right) injections, with recoveries under [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Marginal posteriors on the LOSA parameter [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Joint inference of the LOSA parameter Γ and the orbital eccentricity e at ⟨fref⟩ = 20 Hz for GW200105 162426 (left) and GW190814 (right). Blue contours show 50% and 90% credible regions of the two-dimensional (e, Γ) posterior from SEOBNRv6EHM, with one-dimensional marginals on the side panels. Overlaid are the marginal on e from a SEOBNRv6EHM analysis with Γ fixed to zero (red), and the marginal on Γ from … view at source ↗
read the original abstract

A line-of-sight acceleration (LOSA) of a compact-binary center of mass, imparted for example by a nearby tertiary perturber, imprints a Doppler modulation on the gravitational-wave signal and provides a single-event diagnostic of dynamical formation environments. Waveform-modeling systematics -- missing higher-order modes, spin precession, or orbital eccentricity -- can mimic or mask a non-zero LOSA, making waveform accuracy a leading concern for LOSA inference. We implement LOSA corrections directly in the time domain as a remap of the strain: the treatment applies uniformly to all mode content, spin precession, and orbital eccentricity, and integrates naturally with time-domain inspiral-merger-ringdown models that best capture these effects. We deploy it in the SEOBNRv6EHM (aligned-spin eccentric) and SEOBNRv5PHM (precessing quasi-circular) models, and validate the implementation on simulated signals; we find that SEOBNRv6EHM recovers LOSA correctly on both eccentric and spin-precessing injections, while SEOBNRv5PHM yields a spurious LOSA measurement on eccentric signals. Motivated by the eccentricity hints in the neutron-star--black-hole (NSBH) event GW200105_162426 and the favorable low-mass regime of these sources, we jointly infer LOSA and orbital eccentricity for the five NSBH events in the LIGO-Virgo-KAGRA catalog, reporting the first LOSA constraints on three of them. All five events are consistent with a vanishing LOSA, $\Gamma \equiv a_\parallel/c = 0$; for GW200105_162426, the joint $(\Gamma, e)$ posterior nonetheless disfavors both $\Gamma$ and $e$ being zero simultaneously at 90% credibility, supporting the eccentricity hints reported in previous analyses.

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

1 major / 0 minor

Summary. The paper implements line-of-sight acceleration (LOSA, via Γ ≡ a∥/c) as a time-domain remap of the strain that applies uniformly across modes, precession, and eccentricity. It deploys the correction in SEOBNRv6EHM (aligned-spin eccentric) and SEOBNRv5PHM (precessing quasi-circular), validates recovery on simulated signals (correct with v6EHM, spurious LOSA with v5PHM on eccentric injections), and performs joint LOSA+eccentricity inference on the five NSBH events in the LVK catalog. All five events are reported consistent with Γ=0; the joint (Γ,e) posterior for GW200105_162426 disfavors (Γ=0,e=0) simultaneously at 90% credibility.

Significance. If robust, the work supplies the first LOSA constraints on NSBH binaries and bolsters existing eccentricity indications for GW200105_162426 as a formation-channel diagnostic. The time-domain remapping is a technical strength because it integrates directly with inspiral-merger-ringdown models that already include eccentricity and precession. Validation on simulated signals is explicitly credited as demonstrating differential model performance.

major comments (1)
  1. [Abstract] Abstract: the headline 90% credibility disfavoring of (Γ=0,e=0) for GW200105_162426 is reported without stating which waveform model (SEOBNRv6EHM or SEOBNRv5PHM) was used for that posterior. The manuscript demonstrates that SEOBNRv5PHM returns spurious non-zero LOSA on eccentric injections while SEOBNRv6EHM recovers the injected value correctly; because the joint analysis is motivated by eccentricity hints, the model choice is load-bearing for whether the exclusion is physical or an artifact.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their detailed review and for highlighting the need for clarity in the abstract regarding the waveform model. We address the comment below and will make the requested revision.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the headline 90% credibility disfavoring of (Γ=0,e=0) for GW200105_162426 is reported without stating which waveform model (SEOBNRv6EHM or SEOBNRv5PHM) was used for that posterior. The manuscript demonstrates that SEOBNRv5PHM returns spurious non-zero LOSA on eccentric injections while SEOBNRv6EHM recovers the injected value correctly; because the joint analysis is motivated by eccentricity hints, the model choice is load-bearing for whether the exclusion is physical or an artifact.

    Authors: We agree that the abstract should explicitly identify the waveform model for the joint (Γ, e) posterior on GW200105_162426. This analysis was performed with SEOBNRv6EHM, the aligned-spin eccentric model, because the joint inference targets orbital eccentricity (the SEOBNRv5PHM results are reported separately for the quasi-circular precessing case). We will revise the abstract to state that the joint posterior was obtained with SEOBNRv6EHM, thereby removing any ambiguity about whether the reported 90% credibility exclusion is physical or an artifact of model mismatch. revision: yes

Circularity Check

0 steps flagged

No circularity: posteriors are direct Bayesian outputs from catalog data

full rationale

The paper's central results are joint posteriors on LOSA (Γ) and eccentricity (e) obtained via standard Bayesian sampling of LIGO-Virgo-KAGRA strain data using the implemented LOSA remapping inside SEOBNR models. No equation defines a parameter in terms of the target posterior, no fitted input is relabeled as a prediction, and no self-citation chain is invoked to justify the reported consistency with Γ=0 or the 90% disfavoring of (Γ=0,e=0) for GW200105. Validation on injections is external to the real-event inference and does not reduce the claims to internal definitions. The derivation chain is therefore self-contained against the external strain data.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Abstract-only review; no explicit free parameters, ad-hoc axioms, or new entities are stated. Standard GR waveform assumptions are implicit but not enumerated.

axioms (1)
  • standard math General relativity governs the propagation and generation of gravitational waves from compact binaries
    Foundational assumption required for any waveform model used in the analysis

pith-pipeline@v0.9.1-grok · 5872 in / 1361 out tokens · 47774 ms · 2026-06-29T03:21:05.929852+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

137 extracted references · 3 canonical work pages

  1. [1]

    Analysis of GW200105 162426 For GW200105 162426, multiple independent analyses have indicated signs of non-zero orbital eccentricity, with some sensitivity to prior choices [42, 45, 46, 48, 49, 54]. Ref. [72] additionally reported aΓconstraint with the PN inspiral-only eccentric–precessing modelpyEFPE, finding a broadening of the eccentricity posterior wh...

    arXiv

  2. [2]

    Among the five events, GW190814 is the only one with a previous LOSA claim in the literature: Ref

    Analysis of GW190814 GW190814 has been analyzed several times for LOSA in the recent literature, with conflicting conclusions whose dif- ferences trace to choices of signal duration and waveform modeling systematics; we briefly summarize them before placing our result. Among the five events, GW190814 is the only one with a previous LOSA claim in the liter...

  3. [3]

    Making Sense of the Unexpected in the Gravitational- Wave Sky

    Astrophysical implications The marginalΓposteriors of Table I can be recast as ex- clusion regions on the massM • and separationrof a putative tertiary perturber via Eq. (6) of Ref. [64], Γ≈4.65×10 −12 s−1 M• 1010 M⊙ ! r 1 pc !−2 cosθ,(4) whereθis the angle between the acceleration vector (which, for a spherically symmetric potential, is aligned with the ...

  4. [4]

    Aasi et al.,Advanced LIGO, Class

    LIGO Scientificcollaboration, J. Aasi et al.,Advanced LIGO, Class. Quant. Grav.32(2015) 074001 [1411.4547]

    Pith/arXiv arXiv 2015

  5. [5]

    Acernese et al.,Advanced Virgo: a second-generation interferometric gravitational wave detector,Class

    VIRGO collaboration, F. Acernese et al.,Advanced Virgo: a second-generation interferometric gravitational wave detector,Class. Quant. Grav.32(2015) 024001 [1408.3978]

    Pith/arXiv arXiv 2015

  6. [6]

    Akutsu et al.,Overview of KAGRA: Detector design and construction history,PTEP2021(2021) 05A101 [2005.05574]

    KAGRA collaboration, T. Akutsu et al.,Overview of KAGRA: Detector design and construction history,PTEP2021(2021) 05A101 [2005.05574]

    arXiv 2021

  7. [7]

    LIGO Scientific, Virgocollaboration, B. P. Abbott et al., Observation of Gravitational Waves from a Binary Black Hole Merger,Phys. Rev. Lett.116(2016) 061102 [1602.03837]

    Pith/arXiv arXiv 2016

  8. [8]

    LIGO Scientific, Virgocollaboration, B. P. Abbott et al., 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 (2019) 031040 [1811.12907]

    Pith/arXiv arXiv 2019

  9. [9]

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

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

    Pith/arXiv arXiv 2021

  10. [10]

    Abbott et al., GWTC-2.1: Deep extended catalog of compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run,Phys

    LIGO Scientific, VIRGO collaboration, R. Abbott et al., GWTC-2.1: Deep extended catalog of compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run,Phys. Rev. D109(2024) 022001 [2108.01045]

    Pith/arXiv arXiv 2024

  11. [11]

    Abbott et al.,GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run,Phys

    KAGRA, VIRGO, LIGO Scientificcollaboration, R. Abbott et al.,GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run,Phys. Rev. X13(2023) 041039 [2111.03606]

    Pith/arXiv arXiv 2023

  12. [12]

    LIGO Scientific, VIRGO, KAGRA collaboration, A. G. Abac et al.,GWTC-4.0: Updating the Gravitational-Wave Transient Catalog with Observations from the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run, 2508.18082

    Pith/arXiv arXiv

  13. [13]

    LIGO Scientific, VIRGO, KAGRA collaboration, GWTC-5.0: Observations from the Second Part of the Fourth LIGO-Virgo-KAGRA Observing Run and Updates to the Gravitational-Wave Transient Catalog,2605.27225

    Pith/arXiv arXiv

  14. [14]

    LIGO Scientific, VIRGO, KAGRA collaboration, GWTC-5.0: Population Properties of Merging Compact Binaries,2605.27226

    Pith/arXiv arXiv

  15. [15]

    Peters and J

    P. Peters and J. Mathews,Gravitational radiation from point masses in a Keplerian orbit,Phys.Rev.131(1963) 435

    1963

  16. [16]

    P. C. Peters,Gravitational Radiation and the Motion of Two Point Masses,Phys. Rev.136(1964) B1224

    1964

  17. [17]

    Wen,On the eccentricity distribution of coalescing black hole binaries driven by the Kozai mechanism in globular clusters,Astrophys

    L. Wen,On the eccentricity distribution of coalescing black hole binaries driven by the Kozai mechanism in globular clusters,Astrophys. J.598(2003) 419 [astro-ph/0211492]

    Pith/arXiv arXiv 2003

  18. [18]

    R. M. O’Leary, B. Kocsis and A. Loeb,Gravitational waves from scattering of stellar-mass black holes in galactic nuclei, Mon. Not. Roy. Astron. Soc.395(2009) 2127 [0807.2638]

    Pith/arXiv arXiv 2009

  19. [19]

    Samsing, M

    J. Samsing, M. MacLeod and E. Ramirez-Ruiz,The Formation of Eccentric Compact Binary Inspirals and the Role of Gravitational Wave Emission in Binary-Single Stellar Encounters,Astrophys. J.784(2014) 71 [1308.2964]

    Pith/arXiv arXiv 2014

  20. [20]

    Samsing,Eccentric Black Hole Mergers Forming in Globular Clusters,Phys

    J. Samsing,Eccentric Black Hole Mergers Forming in Globular Clusters,Phys. Rev. D97(2018) 103014 [1711.07452]

    Pith/arXiv arXiv 2018

  21. [21]

    C. L. Rodriguez, P. Amaro-Seoane, S. Chatterjee, K. Kremer, F. A. Rasio, J. Samsing et al.,Post-Newtonian Dynamics in Dense Star Clusters: Formation, Masses, and Merger Rates of Highly-Eccentric Black Hole Binaries,Phys. Rev. D98 (2018) 123005 [1811.04926]

    Pith/arXiv arXiv 2018

  22. [22]

    Zevin, J

    M. Zevin, J. Samsing, C. Rodriguez, C.-J. Haster and E. Ramirez-Ruiz,Eccentric Black Hole Mergers in Dense Star Clusters: The Role of Binary–Binary Encounters, Astrophys. J.871(2019) 91 [1810.00901]

    Pith/arXiv arXiv 2019

  23. [23]

    Samsing, I

    J. Samsing, I. Bartos, D. J. D’Orazio, Z. Haiman, B. Kocsis, N. W. C. Leigh et al.,AGN as potential factories for eccentric black hole mergers,Nature603(2022) 237 [2010.09765]

    arXiv 2022

  24. [24]

    Tagawa, B

    H. Tagawa, B. Kocsis, Z. Haiman, I. Bartos, K. Omukai and J. Samsing,Eccentric Black Hole Mergers in Active Galactic Nuclei,Astrophys. J. Lett.907(2021) L20 [2010.10526]. 13

    arXiv 2021

  25. [25]

    Zevin, I

    M. Zevin, I. M. Romero-Shaw, K. Kremer, E. Thrane and P. D. Lasky,Implications of Eccentric Observations on Binary Black Hole Formation Channels,Astrophys. J. Lett. 921(2021) L43 [2106.09042]

    arXiv 2021

  26. [26]

    Chattopadhyay, J

    D. Chattopadhyay, J. Stegmann, F. Antonini, J. Barber and I. M. Romero-Shaw,Double black hole mergers in nuclear star clusters: eccentricities, spins, masses, and the growth of massive seeds,Mon. Not. Roy. Astron. Soc.526(2023) 4908 [2308.10884]

    arXiv 2023

  27. [27]

    Stegmann and J

    J. Stegmann and J. Klencki,Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution,Astrophys. J. Lett.991(2025) L54 [2506.09121]

    arXiv 2025

  28. [28]

    Rozner, T

    M. Rozner, T. A. Clarke, I. M. Romero-Shaw and J. Samsing, The Universal Eccentricity Distribution for Dynamical Gravitational-Wave Merger Channels,2602.20110

    arXiv

  29. [29]

    Ramos-Buades, A

    A. Ramos-Buades, A. Buonanno, M. Khalil and S. Ossokine, Effective-one-body multipolar waveforms for eccentric binary black holes with nonprecessing spins,Phys. Rev. D 105(2022) 044035 [2112.06952]

    arXiv 2022

  30. [30]

    Khalil, A

    M. Khalil, A. Buonanno, J. Steinhoffand J. Vines, Radiation-reaction force and multipolar waveforms for eccentric, spin-aligned binaries in the effective-one-body formalism,Phys. Rev. D104(2021) 024046 [2104.11705]

    arXiv 2021

  31. [31]

    Gamboa et al.,Accurate waveforms for eccentric, aligned-spin binary black holes: The multipolar effective-one-body model seobnrv5ehm,Phys

    A. Gamboa et al.,Accurate waveforms for eccentric, aligned-spin binary black holes: The multipolar effective-one-body model seobnrv5ehm,Phys. Rev. D112 (2025) 044038 [2412.12823]

    arXiv 2025

  32. [32]

    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(2025) 044037 [2412.12831]

    arXiv 2025

  33. [33]

    Gamboa et al.,Accurate waveforms for generic planar-orbit binary black holes: The multipolar effective-one-body model SEOBNRv6EHM,2605.28715

    A. Gamboa et al.,Accurate waveforms for generic planar-orbit binary black holes: The multipolar effective-one-body model SEOBNRv6EHM,2605.28715

    Pith/arXiv arXiv

  34. [34]

    Chiaramello and A

    D. Chiaramello and A. Nagar,Faithful analytical effective-one-body waveform model for spin-aligned, moderately eccentric, coalescing black hole binaries,Phys. Rev. D101(2020) 101501 [2001.11736]

    arXiv 2020

  35. [35]

    Nagar, A

    A. Nagar, A. Bonino and P. Rettegno,Effective one-body multipolar waveform model for spin-aligned, quasicircular, eccentric, hyperbolic black hole binaries,Phys. Rev. D103 (2021) 104021 [2101.08624]

    arXiv 2021

  36. [36]

    Nagar, D

    A. Nagar, D. Chiaramello, R. Gamba, S. Albanesi, S. Bernuzzi, V . Fantini et al.,Effective-one-body waveform model for noncircularized, planar, coalescing black hole binaries. II. High accuracy by improving logarithmic terms in resummations,Phys. Rev. D111(2025) 064050 [2407.04762]

    arXiv 2025

  37. [37]

    Albanesi, R

    S. Albanesi, R. Gamba, S. Bernuzzi, J. Fontbut ´e, A. Gonzalez and A. Nagar,Effective-one-body modeling for generic compact binaries with arbitrary orbits,Phys. Rev. D112 (2025) L121503 [2503.14580]

    arXiv 2025

  38. [38]

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

    arXiv 2026

  39. [39]

    Ramos-Buades, Q

    A. Ramos-Buades, Q. Henry and M. Haney,Fast frequency-domain phenomenological modeling of eccentric aligned-spin binary black holes,2601.03340

    arXiv

  40. [40]

    Klein, Y

    A. Klein, Y . Boetzel, A. Gopakumar, P. Jetzer and L. de Vittori,Fourier domain gravitational waveforms for precessing eccentric binaries,Phys. Rev. D98(2018) 104043 [1801.08542]

    Pith/arXiv arXiv 2018

  41. [41]

    Morras, G

    G. Morras, G. Pratten and P. Schmidt,Improved post-Newtonian waveform model for inspiralling precessing-eccentric compact binaries,Phys. Rev. D111 (2025) 084052 [2502.03929]

    arXiv 2025

  42. [42]

    Morras, G

    G. Morras, G. Pratten, P. Schmidt and A. Buonanno, Post-Newtonian inspiral waveform model for eccentric precessing binaries with higher-order modes and matter effects,2604.11903

    Pith/arXiv arXiv

  43. [43]

    P. J. Nee et al.,Eccentric binary black holes: A new framework for numerical relativity waveform surrogates, 2510.00106

    arXiv

  44. [44]

    Islam et al.,Including higher-order modes in a quadrupolar eccentric numerical relativity surrogate using universal eccentric modulation functions,2604.17868

    T. Islam et al.,Including higher-order modes in a quadrupolar eccentric numerical relativity surrogate using universal eccentric modulation functions,2604.17868

    Pith/arXiv arXiv

  45. [45]

    Pompili, A

    L. Pompili, A. Gamboa and A. Buonanno,Eccentric and unbound compact binaries in the LIGO-Virgo-KAGRA catalog: parameter estimation and waveform systematics with SEOBNRv6EHM,2605.28716

    Pith/arXiv arXiv

  46. [46]

    I. M. Romero-Shaw, P. D. Lasky and E. Thrane,Four Eccentric Mergers Increase the Evidence that LIGO–Virgo–KAGRA’s Binary Black Holes Form Dynamically,Astrophys. J.940(2022) 171 [2206.14695]

    arXiv 2022

  47. [47]

    Gupte et al.,Evidence for eccentricity in the population of binary black holes observed by LIGO-Virgo-KAGRA,Phys

    N. Gupte et al.,Evidence for eccentricity in the population of binary black holes observed by LIGO-Virgo-KAGRA,Phys. Rev. D112(2025) 104045 [2404.14286]

    Pith/arXiv arXiv 2025

  48. [48]

    Morras, G

    G. Morras, G. Pratten and P. Schmidt,Orbital eccentricity in a neutron star - black hole binary merger,Astrophys. J. Lett. 1000(2026) L2 [2503.15393]

    arXiv 2026

  49. [49]

    M. d. L. Planas, S. Husa, A. Ramos-Buades and J. Valencia, First Eccentric Inspiral–Merger–Ringdown Analysis of Neutron Star–Black Hole Mergers,Astrophys. J.995(2025) 47 [2506.01760]

    arXiv 2025

  50. [50]

    M. d. L. Planas, A. Ramos-Buades, C. Garc ´ıa-Quir´os, H. Estell´es, S. Husa and M. Haney,Reanalysis of binary black hole gravitational wave events for orbital eccentricity signatures,Phys. Rev. D112(2025) 123004 [2504.15833]

    arXiv 2025

  51. [51]

    Jan, B.-J

    A. Jan, B.-J. Tsao, R. O’Shaughnessy, D. Shoemaker and P. Laguna,GW200105: A detailed study of eccentricity in the neutron star-black hole binary,Phys. Rev. D113(2026) 024018 [2508.12460]

    arXiv 2026

  52. [52]

    Kacanja, K

    K. Kacanja, K. Soni and A. H. Nitz,Eccentricity signatures in LIGO-Virgo-KAGRA’s binary neutron star and neutron-star black holes,Phys. Rev. D112(2025) 122007 [2508.00179]

    arXiv 2025

  53. [53]

    Gupte et al.,Eccentricity constraints disfavor single-single capture in nuclear star clusters as the origin of all LIGO-Virgo-KAGRA binary black holes,2603.29019

    N. Gupte et al.,Eccentricity constraints disfavor single-single capture in nuclear star clusters as the origin of all LIGO-Virgo-KAGRA binary black holes,2603.29019

    arXiv

  54. [54]

    Malagon and R

    N. Malagon and R. O’Shaughnessy,Assessing the imprint of eccentricity in GW signatures using two independent waveform models,2605.12818

    Pith/arXiv arXiv

  55. [55]

    I. M. Romero-Shaw, D. Gerosa and N. Loutrel,Eccentricity or spin precession? Distinguishing subdominant effects in gravitational-wave data,Mon. Not. Roy. Astron. Soc.519 (2023) 5352 [2211.07528]

    arXiv 2023

  56. [56]

    Calder ´on Bustillo, N

    J. Calder ´on Bustillo, N. Sanchis-Gual, A. Torres-Forn´e and J. A. Font,Confusing Head-On Collisions with Precessing Intermediate-Mass Binary Black Hole Mergers,Phys. Rev. Lett.126(2021) 201101 [2009.01066]

    arXiv 2021

  57. [57]

    T. A. Clarke, I. M. Romero-Shaw, C. Hoy, J. Stegmann, P. D. Lasky and E. Thrane,A universal framework to identify eccentric binary mergers: GW200105 case study, 2605.18742. 14

    Pith/arXiv arXiv

  58. [58]

    A. Jan, S. Nicolella, D. Shoemaker and R. O’Shaughnessy, Measuring Eccentricity and Addressing Waveform Systematics in GW231123,2512.20060

    Pith/arXiv arXiv

  59. [59]

    Yunes, M

    N. Yunes, M. Coleman Miller and J. Thornburg,The Effect of Massive Perturbers on Extreme Mass-Ratio Inspiral Waveforms,Phys. Rev. D83(2011) 044030 [1010.1721]

    Pith/arXiv arXiv 2011

  60. [60]

    Meiron, B

    Y . Meiron, B. Kocsis and A. Loeb,Detecting triple systems with gravitational wave observations,Astrophys. J.834 (2017) 200 [1604.02148]

    Pith/arXiv arXiv 2017

  61. [61]

    Inayoshi, N

    K. Inayoshi, N. Tamanini, C. Caprini and Z. Haiman,Probing stellar binary black hole formation in galactic nuclei via the imprint of their center of mass acceleration on their gravitational wave signal,Phys. Rev. D96(2017) 063014 [1702.06529]

    Pith/arXiv arXiv 2017

  62. [62]

    Robson, N

    T. Robson, N. J. Cornish, N. Tamanini and S. Toonen, Detecting hierarchical stellar systems with LISA,Phys. Rev. D98(2018) 064012 [1806.00500]

    Pith/arXiv arXiv 2018

  63. [63]

    Toubiana et al.,Detectable environmental effects in GW190521-like black-hole binaries with LISA,Phys

    A. Toubiana et al.,Detectable environmental effects in GW190521-like black-hole binaries with LISA,Phys. Rev. Lett.126(2021) 101105 [2010.06056]

    arXiv 2021

  64. [64]

    Samsing, K

    J. Samsing, K. Hendriks, L. Zwick, D. J. D’Orazio and B. Liu,Gravitational Wave Phase Shifts in Eccentric Black Hole Mergers as a Probe of Dynamical Formation Environments,2403.05625

    arXiv

  65. [65]

    Hendriks, L

    K. Hendriks, L. Zwick and J. Samsing,Eccentric Features in the Gravitational-wave Phase of Dynamically Formed Black Hole Binaries,Astrophys. J.985(2025) 252 [2408.04603]

    arXiv 2025

  66. [66]

    Bonvin, C

    C. Bonvin, C. Caprini, R. Sturani and N. Tamanini,Effect of matter structure on the gravitational waveform,Phys. Rev. D 95(2017) 044029 [1609.08093]

    Pith/arXiv arXiv 2017

  67. [67]

    Vijaykumar, A

    A. Vijaykumar, A. Tiwari, S. J. Kapadia, K. G. Arun and P. Ajith,Waltzing Binaries: Probing the Line-of-sight Acceleration of Merging Compact Objects with Gravitational Waves,Astrophys. J.954(2023) 105 [2302.09651]

    arXiv 2023

  68. [68]

    Barausse, V

    E. Barausse, V . Cardoso and P. Pani,Can environmental effects spoil precision gravitational-wave astrophysics?, Phys.Rev.D89(2014) 104059 [1404.7149]

    Pith/arXiv arXiv 2014

  69. [69]

    Zwick, K

    L. Zwick, K. Hendriks, P. Saini, J. Tak´atsy, C. Rowan, J. Samsing et al.,Environmental effects in stellar mass gravitational wave sources II: Joint detections of eccentricity and phase shifts in binary sub-populations,2511.04540

    arXiv

  70. [70]

    Tagawa, C

    H. Tagawa, C. Rowan, J. Tak´atsy, L. Zwick, K. Hendriks, W.-B. Han et al.,Gravitational Wave Phase Shifts of Black Hole Mergers in AGN Disks,Astrophys. J.998(2026) 244 [2511.15193]

    arXiv 2026

  71. [71]

    Tak ´atsy, L

    J. Tak ´atsy, L. Zwick, K. Hendriks, P. Saini, G. Fabj and J. Samsing,The construction and use of dephasing prescriptions for environmental effects in gravitational wave astronomy,Class. Quant. Grav.42(2025) 215006 [2505.09513]

    arXiv 2025

  72. [72]

    Krolak, K

    A. Krolak, K. D. Kokkotas and G. Schaefer,On estimation of the postNewtonian parameters in the gravitational wave emission of a coalescing binary,Phys. Rev. D52(1995) 2089 [gr-qc/9503013]

    Pith/arXiv arXiv 1995

  73. [73]

    S. A. Bhat, A. Tiwari, M. A. Shaikh and S. J. Kapadia, Eccentricity evolution consistency test to distinguish eccentric gravitational-wave signals from eccentricity mimickers,Phys. Rev. D112(2025) 124004 [2508.14850]

    arXiv 2025

  74. [74]

    Pathak, H

    L. Pathak, H. Phurailatpam and A. Gopakumar,On the Presence of a Tertiary Compact Object in GW190814, 2605.21955

    Pith/arXiv arXiv

  75. [75]

    Roy and J

    S. Roy and J. Janquart,Line-of-sight acceleration in compact binaries with higher harmonics and eccentricity, 2606.08838

    Pith/arXiv arXiv

  76. [76]

    Sberna et al.,Observing GW190521-like binary black holes and their environment with LISA,Phys

    L. Sberna et al.,Observing GW190521-like binary black holes and their environment with LISA,Phys. Rev. D106 (2022) 064056 [2205.08550]

    arXiv 2022

  77. [77]

    Tiwari, A

    A. Tiwari, A. Vijaykumar, S. J. Kapadia, S. Ghosh and A. B. Nielsen,A pipeline to search for signatures of line-of-sight acceleration in gravitational wave signals produced by compact binary coalescences,2506.22272

    Pith/arXiv arXiv

  78. [78]

    Hendriks, L

    K. Hendriks, L. Zwick, P. Saini, J. Tak´atsy and J. Samsing, Towards gravitational wave parameter inference for binaries with an eccentric companion,2601.14918

    arXiv

  79. [79]

    LIGO Scientific, VIRGO, KAGRA collaboration, A. G. Abac et al.,GWTC-4.0: Tests of General Relativity. II. Parameterized Tests,2603.19020

    Pith/arXiv arXiv

  80. [80]

    Yang, W.-B

    S.-C. Yang, W.-B. Han, H. Tagawa, S. Li, Y . Jiang, P. Shen et al.,Indication for a Compact Object Next to a LIGO–Virgo Binary Black Hole Merger,Astrophys. J. Lett.988(2025) L41 [2401.01743]

    arXiv 2025

Showing first 80 references.