pith. sign in

arxiv: 2606.08838 · v1 · pith:FWL4IZB5new · submitted 2026-06-07 · 🌀 gr-qc · astro-ph.HE

Line-of-sight acceleration in compact binaries with higher harmonics and eccentricity

Soumen Roy , Justin Janquart This is my paper

Pith reviewed 2026-06-27 17:39 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.HE
keywords gravitational wavescompact binariesline-of-sight accelerationhigher-order modeseccentricitywaveform modelingenvironmental effectsbinary formation
0
0 comments X

The pith

Line-of-sight acceleration must be applied consistently to all harmonics to avoid biased parameter estimates in gravitational-wave signals.

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

This work re-derives line-of-sight acceleration effects and adds them to waveform models that include precession and higher-order modes for quasi-circular binaries as well as to eccentric models. The corrections are imposed on every harmonic in the same way. Tests on events from LIGO and Virgo's third observing run show no clear acceleration signal, but reveal that applying the effect differently to different harmonics can distort the inferred parameters. The resulting model supplies a reliable way to search for environmental influences on binary origins in ongoing and upcoming observations.

Core claim

We re-derive the line-of-sight acceleration effects and implement them in state-of-the-art quasi-circular waveform models with precession and higher-order modes. We also implement the corrections in eccentric waveform models, applying them consistently to all contributing harmonics. Using this model, we investigate the impact of these effects on the inference of line-of-sight acceleration and analyze a few interesting GWTC events observed during the third observing run of LIGO and Virgo. We find no substantial evidence for line-of-sight acceleration in these events. We also show that an inconsistent treatment of line-of-sight acceleration between higher harmonics can lead to biased conclusio

What carries the argument

line-of-sight acceleration phase correction applied uniformly to every harmonic in the waveform

If this is right

  • An inconsistent treatment of the acceleration between different harmonics produces biased parameter estimates.
  • The model can be used to search for environmental signatures in current and future gravitational-wave data.
  • Analysis of third-observing-run events yields no substantial evidence for line-of-sight acceleration.
  • Uniform application across harmonics supports more accurate probes of compact-binary formation channels.

Where Pith is reading between the lines

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

  • This consistency requirement may extend to modeling other dynamical effects in waveforms.
  • With larger event catalogs, the framework could help separate formation channels based on acceleration measurements.
  • Similar modeling consistency might be needed for space-based detectors observing lower-frequency binaries.

Load-bearing premise

Line-of-sight acceleration effects apply uniformly to all harmonics in the waveform without creating inference biases when treated consistently.

What would settle it

Recovering different values for the line-of-sight acceleration parameter from the same data when the correction is applied uniformly versus non-uniformly to the harmonics.

Figures

Figures reproduced from arXiv: 2606.08838 by Justin Janquart, Soumen Roy.

Figure 1
Figure 1. Figure 1: FIG. 1. Systematic biases in [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Illustrating [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Fractional [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Comparison of the marginalized posterior distributions for [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Marginalized posterior distributions from the [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Marginalized posterior distributions for the acceleration pa [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: shows the recovered posteriors obtained with these two approximate prescriptions, compared to the fully consis￾tent PhenomXPHM implementation as also shown in [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗
read the original abstract

Direct detections of gravitational waves provide a unique opportunity to probe the astrophysical origin of compact binary mergers. The formation channels of these systems remain highly debated, and a fraction may originate in dynamical environments or active galactic nuclei. Binaries formed in such environments are expected to experience line-of-sight acceleration from their surroundings, which can imprint characteristic signatures on the observed gravitational-wave signal. Here, we re-derive the line-of-sight acceleration effects and implement them in state-of-the-art quasi-circular waveform models with precession and higher-order modes. We also implement the corrections in eccentric waveform models, applying them consistently to all contributing harmonics. Using this model, we investigate the impact of these effects on the inference of line-of-sight acceleration and analyze a few interesting GWTC events observed during the third observing run of LIGO and Virgo. We find no substantial evidence for line-of-sight acceleration in these events. We also show that an inconsistent treatment of line-of-sight acceleration between higher harmonics can lead to biased conclusions. Our model provides a robust framework for uncovering line-of-sight acceleration in current and future gravitational-wave observations, enabling more accurate probes of environmental signatures in compact-binary formation.

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 / 3 minor

Summary. The paper re-derives line-of-sight acceleration effects on gravitational-wave signals from compact binaries and implements the corrections consistently across all harmonics in state-of-the-art quasi-circular waveform models (including precession and higher-order modes) as well as in eccentric models. The authors apply the resulting model to a selection of GWTC-3 events, report no substantial evidence for line-of-sight acceleration, demonstrate that inconsistent treatment of higher harmonics produces biased inference, and position the framework as a tool for future environmental probes.

Significance. If the implementation and bias demonstration hold, the work supplies a practical, consistently formulated correction that can be used in current and next-generation GW analyses to test for environmental signatures in binary formation. The explicit comparison of consistent versus inconsistent harmonic treatments is a concrete, falsifiable contribution that strengthens the case for including such effects in parameter estimation.

minor comments (3)
  1. [Abstract / §3] The abstract refers to 'a few interesting GWTC events' without stating the selection criteria or the number of events examined; this should be stated explicitly in §3 or §4 with a table listing the events and their posterior constraints on the acceleration parameter.
  2. [§2] Notation for the line-of-sight acceleration parameter (denoted variously as a_LOS or similar) should be unified throughout; the current usage mixes symbols between the re-derivation and the waveform implementation sections.
  3. [Figure 4] Figure captions for the bias demonstration plots should include the injected values and the recovered posterior means with 90% credible intervals so that the magnitude of the bias is immediately quantifiable.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive summary and recommendation of minor revision. No specific major comments were provided in the report, so we have no individual points to address. We are pleased that the referee recognizes the value of consistent implementation across harmonics and the demonstration of bias from inconsistent treatment.

Circularity Check

0 steps flagged

No significant circularity identified

full rationale

The abstract describes re-deriving line-of-sight acceleration effects, implementing them consistently across harmonics in quasi-circular and eccentric waveform models, analyzing GWTC events, and demonstrating bias from inconsistent treatment. No load-bearing step reduces by construction to a fitted parameter, self-definition, or self-citation chain; the central claims rest on implementation details and external data analysis rather than tautological renaming or imported uniqueness theorems. This matches the default expectation of a self-contained derivation against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No information available from abstract alone to identify free parameters, axioms or invented entities.

pith-pipeline@v0.9.1-grok · 5737 in / 993 out tokens · 23387 ms · 2026-06-27T17:39:45.031661+00:00 · methodology

discussion (0)

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

Forward citations

Cited by 1 Pith paper

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

  1. Constraints on Line-of-Sight Acceleration from O1-O4

    astro-ph.HE 2026-06 unverdicted novelty 6.0

    All known compact binary mergers show line-of-sight accelerations consistent with zero under a new time-domain Doppler-shift model, with current detectors only sensitive to high-acceleration scenarios.

Reference graph

Works this paper leans on

92 extracted references · 43 linked inside Pith · cited by 1 Pith paper

  1. [1]

    shows theLoSAresult obtained with the PhenomXPHMmodel when theLoSAcorrection is computed using a quadrupolarprescriptionandapplieduniformlyacrossthefullhigher- harmonic waveform, similar to Ref. [85]. The inconsistent applica- tion ofLoSAcorrection in the higher-order modes can lead to a re- duction in the support for a non-zeroΓ. favoroftheLoSAhypothesis...

  2. [2]

    Aasiet al.(LIGO Scientific),Advanced LIGO, Class

    J. Aasiet al.(LIGO Scientific),Advanced LIGO, Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]

    Pith/arXiv arXiv 2015

  3. [3]

    Acerneseet al.(VIRGO),Advanced Virgo: a second- generation interferometric gravitational wave detector, Class

    F. Acerneseet al.(VIRGO),Advanced Virgo: a second- generation interferometric gravitational wave detector, Class. 14 Quant. Grav.32, 024001 (2015), arXiv:1408.3978 [gr-qc]

    Pith/arXiv arXiv 2015

  4. [4]

    Akutsuet al.(KAGRA),Overview of KAGRA: Detector de- sign and construction history, PTEP2021, 05A101 (2021), arXiv:2005.05574 [physics.ins-det]

    T. Akutsuet al.(KAGRA),Overview of KAGRA: Detector de- sign and construction history, PTEP2021, 05A101 (2021), arXiv:2005.05574 [physics.ins-det]

    arXiv 2021

  5. [5]

    The LIGO Scientific Collaboration, the Virgo Collaboration, andtheKAGRACollaboration,GWTC-5.0: Observationsfrom the Second Part of the Fourth LIGO-Virgo-KAGRA Observing Run and Updates to the Gravitational-Wave Transient Catalog, arXiv e-prints , arXiv:2605.27225 (2026), arXiv:2605.27225 [gr-qc]

    Pith/arXiv arXiv 2026

  6. [6]

    A.G.Abacetal.(LIGOScientific, VIRGO,KAGRA),GWTC- 4.0: Updating the Gravitational-Wave Transient Catalog with Observations from the First Part of the Fourth LIGO-Virgo- KAGRA Observing Run, arXiv e-prints , arXiv:2508.18082 (2025), arXiv:2508.18082 [gr-qc]

    Pith/arXiv arXiv 2025

  7. [7]

    Abbottet al.(KAGRA, VIRGO, LIGO Scientific),GWTC- 3: CompactBinaryCoalescencesObservedbyLIGOandVirgo during the Second Part of the Third Observing Run, Phys

    R. Abbottet al.(KAGRA, VIRGO, LIGO Scientific),GWTC- 3: CompactBinaryCoalescencesObservedbyLIGOandVirgo during the Second Part of the Third Observing Run, Phys. Rev. X13, 041039 (2023), arXiv:2111.03606 [gr-qc]

    Pith/arXiv arXiv 2023

  8. [8]

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

    Pith/arXiv arXiv 2021

  9. [9]

    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

  10. [10]

    Dhurkunde, and C

    A.H.Nitz,S.Kumar,Y.-F.Wang,S.Kastha,S.Wu,M.Schäfer, R. Dhurkunde, and C. D. Capano,4-OGC: Catalog of Gravita- tionalWaves fromCompactBinary Mergers,Astrophys. J.946, 59 (2023), arXiv:2112.06878 [astro-ph.HE]

    arXiv 2023

  11. [11]

    Wadekar, J

    D. Wadekar, J. Roulet, T. Venumadhav, A. K. Mehta, B. Za- ckay, J. Mushkin, S. Olsen, and M. Zaldarriaga,New black hole mergers in the LIGO-Virgo O3 data from a gravitational wavesearchincludinghigher-orderharmonics,arXive-prints, arXiv:2312.06631 (2023), arXiv:2312.06631 [gr-qc]

    arXiv 2023

  12. [12]

    19, 1 (2016), arXiv:1304.0670 [gr-qc]

    B.P.Abbottetal.(KAGRA,LIGOScientific,Virgo),Prospects for observing and localizing gravitational-wave transients with AdvancedLIGO,AdvancedVirgoandKAGRA,LivingRev.Rel. 19, 1 (2016), arXiv:1304.0670 [gr-qc]

    Pith/arXiv arXiv 2016

  13. [13]

    A.G.Abacetal.(LIGOScientific, VIRGO,KAGRA),GWTC- 4.0: PopulationPropertiesofMergingCompactBinaries,arXiv e-prints , arXiv:2508.18083 (2025), arXiv:2508.18083 [astro- ph.HE]

    Pith/arXiv arXiv 2025

  14. [14]

    R. Abbottet al.(KAGRA, VIRGO, LIGO Scientific),Popu- lation of Merging Compact Binaries Inferred Using Gravita- tionalWavesthroughGWTC-3,Phys.Rev.X13,011048(2023), arXiv:2111.03634 [astro-ph.HE]

    Pith/arXiv arXiv 2023

  15. [15]

    Antonelli, K

    A. Antonelli, K. Kritos, K. K. Y. Ng, R. Cotesta, and E. Berti, Classifying the generation and formation channels of individ- ualLIGO-Virgo-KAGRAobservationsfromdynamicallyformed binaries, Phys. Rev. D108, 084044 (2023), arXiv:2306.11088 [gr-qc]

    arXiv 2023

  16. [16]

    C. L. Rodriguez, S. Chatterjee, and F. A. Rasio,Binary Black Hole Mergers from Globular Clusters: Masses, Merger Rates, and the Impact of Stellar Evolution, Phys. Rev. D93, 084029 (2016), arXiv:1602.02444 [astro-ph.HE]

    Pith/arXiv arXiv 2016

  17. [17]

    Mapelli, Y

    M. Mapelli, Y. Bouffanais, F. Santoliquido, M. A. Sedda, and M. C. Artale,The cosmic evolution of binary black holes in young,globular,andnuclearstarclusters: rates,masses,spins, and mixing fractions, Mon. Not. Roy. Astron. Soc.511, 5797– 5816 (2022), arXiv:2109.06222 [astro-ph.HE]

    arXiv 2022

  18. [18]

    Antonini, S

    F. Antonini, S. Toonen, and A. S. Hamers,Binary black hole mergers from field triples: properties, rates and the impact of stellar evolution, Astrophys. J.841, 77 (2017), arXiv:1703.06614 [astro-ph.GA]

    Pith/arXiv arXiv 2017

  19. [19]

    Silsbee and S

    K. Silsbee and S. Tremaine,Lidov-Kozai Cycles with Gravita- tional Radiation: Merging Black Holes in Isolated Triple Sys- tems, Astrophys. J.836, 39 (2017), arXiv:1608.07642 [astro- ph.HE]

    Pith/arXiv arXiv 2017

  20. [20]

    J.863, 68 (2018), arXiv:1805.03202 [astro- ph.HE]

    B.LiuandD.Lai,BlackHoleandNeutronStarBinaryMergers in Triple Systems: Merger Fraction and Spin–Orbit Misalign- ment, Astrophys. J.863, 68 (2018), arXiv:1805.03202 [astro- ph.HE]

    Pith/arXiv arXiv 2018

  21. [21]

    J.835, 165 (2017), arXiv:1602.03831 [astro- ph.HE]

    I.Bartos,B.Kocsis,Z.Haiman,andS.Márka,RapidandBright Stellar-mass Binary Black Hole Mergers in Active Galactic Nu- clei, Astrophys. J.835, 165 (2017), arXiv:1602.03831 [astro- ph.HE]

    Pith/arXiv arXiv 2017

  22. [22]

    McKernan, K

    B. McKernan, K. E. S. Ford, and R. O’Shaughnessy,Black hole, neutron star, and white dwarf merger rates in AGN discs, Mon. Not. Roy. Astron. Soc.498, 4088–4094 (2020), arXiv:2002.00046 [astro-ph.HE]

    arXiv 2020

  23. [23]

    Rowan, T

    C. Rowan, T. Boekholt, B. Kocsis, and Z. Haiman,Black hole binary formation in AGN discs: from isolation to merger, Mon. Not. Roy. Astron. Soc.524, 2770–2796 (2023), arXiv:2212.06133 [astro-ph.GA]

    arXiv 2023

  24. [24]

    Lasky,ImplicationsofEccentricObservationsonBinaryBlack Hole Formation Channels, Astrophys

    M.Zevin, I.M.Romero-Shaw, K.Kremer, E.Thrane,andP.D. Lasky,ImplicationsofEccentricObservationsonBinaryBlack Hole Formation Channels, Astrophys. J. Lett.921, L43 (2021), arXiv:2106.09042 [astro-ph.HE]

    arXiv 2021

  25. [25]

    Dall’Amico, M

    M. Dall’Amico, M. Mapelli, S. Torniamenti, and M. A. Sedda, Eccentric black hole mergers via three-body interactions in young, globular, and nuclear star clusters, Astron. Astrophys. 683, A186 (2024), arXiv:2303.07421 [astro-ph.HE]

    arXiv 2024

  26. [26]

    Stegmann, D

    J. Stegmann, D. Gerosa, I. Romero-Shaw, G. Fumagalli, H. Tagawa, and L. Zwick,Distinguishing the Origin of Eccen- tricBlackHoleMergerswithGravitational-waveSpinMeasure- ments, Astrophys. J. Lett.994, L47 (2025), arXiv:2505.13589 [astro-ph.HE]

    arXiv 2025

  27. [27]

    Fumagalli and D

    G. Fumagalli and D. Gerosa,Spin-eccentricity interplay in merging binary black holes, Phys. Rev. D108, 124055 (2023), arXiv:2310.16893 [gr-qc]

    arXiv 2023

  28. [28]

    P. C. Peters,Gravitational Radiation and the Motion of Two Point Masses, Phys. Rev.136, B1224–B1232 (1964)

    1964

  29. [29]

    Tucker and C

    A. Tucker and C. M. Will,Residual eccentricity of inspiralling orbits at the gravitational-wave detection threshold: Accu- rate estimates using post-Newtonian theory, Phys. Rev. D104, 104023 (2021), arXiv:2108.12210 [gr-qc]

    arXiv 2021

  30. [30]

    Calderón Bustillo, N

    J. Calderón Bustillo, N. Sanchis-Gual, A. Torres-Forné, and J. A. Font,Confusing Head-On Collisions with Precessing Intermediate-MassBinaryBlackHoleMergers,Phys.Rev.Lett. 126, 201101 (2021), arXiv:2009.01066 [gr-qc]

    arXiv 2021

  31. [31]

    Romero-Shaw, J

    I. Romero-Shaw, J. Stegmann, H. Tagawa, D. Gerosa, J. Sam- sing, N. Gupte, and S. R. Green,GW200208_222617 as an eccentric black-hole binary merger: Properties and as- trophysical implications, Phys. Rev. D112, 063052 (2025), arXiv:2506.17105 [astro-ph.HE]

    arXiv 2025

  32. [32]

    Divyajyotiet al.,Biased parameter inference of eccen- tric, spin-precessing binary black holes, arXiv e-prints , arXiv:2510.04332 (2025), arXiv:2510.04332 [gr-qc]

    Pith/arXiv arXiv 2025

  33. [33]

    Tibrewal, A

    S. Tibrewal, A. Zimmerman, J. Lange, and D. Shoemaker, 15 Misinterpreting Spin Precession as Orbital Eccentricity in Gravitational-Wave Signals, arXiv e-prints , arXiv:2601.02260 (2026), arXiv:2601.02260 [gr-qc]

    arXiv 2026

  34. [34]

    Takahashi and T

    R. Takahashi and T. Nakamura,Determination of the equation of the state of the universe using ~ 0.1 Hz gravitational wave detectors, Prog. Theor. Phys.113, 63–71 (2005), arXiv:astro- ph/0408547

    arXiv 2005

  35. [35]

    Yunes, M

    N. Yunes, M. Coleman Miller, and J. Thornburg,The Effect of Massive Perturbers on Extreme Mass-Ratio Inspiral Wave- forms,Phys.Rev.D83,044030(2011),arXiv:1010.1721[astro- ph.GA]

    Pith/arXiv arXiv 2011

  36. [36]

    Y.Meiron,B.Kocsis,andA.Loeb,Detectingtriplesystemswith gravitationalwaveobservations,Astrophys.J.834,200(2017), arXiv:1604.02148 [astro-ph.HE]

    Pith/arXiv arXiv 2017

  37. [37]

    Bonvin, C

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

    Pith/arXiv arXiv 2017

  38. [38]

    Inayoshi, N

    K. Inayoshi, N. Tamanini, C. Caprini, and Z. Haiman,Probing stellarbinaryblackholeformationingalacticnucleiviatheim- print of their center of mass acceleration on their gravitational wavesignal,Phys.Rev.D96,063014(2017),arXiv:1702.06529 [astro-ph.HE]

    Pith/arXiv arXiv 2017

  39. [39]

    Tamanini, A

    N. Tamanini, A. Klein, C. Bonvin, E. Barausse, and C.Caprini, Peculiar acceleration of stellar-origin black hole binaries: Measurement and biases with LISA, Phys. Rev. D101, 063002 (2020), arXiv:1907.02018 [astro-ph.IM]

    arXiv 2020

  40. [40]

    Vijaykumar, A

    A. Vijaykumar, A. Tiwari, S. J. Kapadia, K. G. Arun, and P. Ajith,Waltzing Binaries: Probing the Line-of-sight Accel- erationofMergingCompactObjectswithGravitationalWaves, Astrophys.J.954,105(2023),arXiv:2302.09651[astro-ph.HE]

    arXiv 2023

  41. [41]

    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 ac- celeration in gravitational wave signals produced by compact binarycoalescences,arXive-prints,arXiv:2506.22272(2025), arXiv:2506.22272 [astro-ph.HE]

    Pith/arXiv arXiv 2025

  42. [42]

    Tiwari, A

    A. Tiwari, A. Vijaykumar, S. J. Kapadia, S. Chatterjee, and G. Fragione,Profiling stellar environments of gravi- tational wave sources, Phys. Rev. D112, 084034 (2025), arXiv:2407.15117 [astro-ph.HE]

    arXiv 2025

  43. [43]

    Lazarow, N

    M. Lazarow, N. Leslie, and L. Dai,Gravitational waveform modelfordetectingacceleratinginspiralingbinaries,Phys.Rev. D110, 083008 (2024), arXiv:2401.04175 [gr-qc]

    arXiv 2024

  44. [44]

    Gera and P

    S. Gera and P. Dutta Roy,Impact of neglecting center- of-mass acceleration in parameter estimation of stellar- mass black holes, arXiv e-prints , arXiv:2512.21979 (2025), arXiv:2512.21979 [gr-qc]

    arXiv 2025

  45. [45]

    Samsing, K

    J. Samsing, K. Hendriks, L. Zwick, D. J. D’Orazio, and B. Liu, Gravitational-wavePhaseShiftsinEccentricBlackHoleMerg- ers as a Probe of Dynamical Formation Environments, Astro- phys. J.990, 211 (2025), arXiv:2403.05625 [astro-ph.HE]

    arXiv 2025

  46. [46]

    Hendriks, L

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

    arXiv 2025

  47. [47]

    Tiwari, A

    A. Tiwari, A. Vijaykumar, S. J. Kapadia, G. Fragione, and S. Chatterjee,Accelerated binary black holes in globular clus- ters: forecasts and detectability in the era of space-based gravitational-wave detectors, Mon. Not. Roy. Astron. Soc.527, 8586–8597 (2023), arXiv:2307.00930 [astro-ph.HE]

    arXiv 2023

  48. [48]

    S. H. W. Leong, J. Janquart, A. K. Sharma, P. Martens, P. Ajith, and O. A. Hannuksela,Constraining Binary Merg- ers in Active Galactic Nuclei Disks Using the Nonobservation of Lensed Gravitational Waves, Astrophys. J. Lett.979, L27 (2025), arXiv:2408.13144 [astro-ph.HE]

    arXiv 2025

  49. [49]

    Chamberlain, C

    K. Chamberlain, C. J. Moore, D. Gerosa, and N. Yunes, Frequency-domain waveform approximants capturing Doppler shifts, Phys. Rev. D99, 024025 (2019), arXiv:1809.04799 [gr- qc]

    Pith/arXiv arXiv 2019

  50. [50]

    A.G.Abacetal.(LIGOScientific, VIRGO,KAGRA),GWTC- 4.0: Tests of General Relativity. II. Parameterized Tests, arXiv e-prints , arXiv:2603.19020 (2026), arXiv:2603.19020 [gr-qc]

    Pith/arXiv arXiv 2026

  51. [51]

    Damour, B

    T. Damour, B. R. Iyer, and B. S. Sathyaprakash,A Comparison of search templates for gravitational waves from binary inspi- ral, Phys. Rev. D63, 044023 (2001), [Erratum: Phys.Rev.D 72, 029902 (2005)], arXiv:gr-qc/0010009

    Pith/arXiv arXiv 2001

  52. [52]

    Buonanno, B

    A. Buonanno, B. Iyer, E. Ochsner, Y. Pan, and B. S. Sathyaprakash,Comparison of post-Newtonian templates for compactbinaryinspiralsignalsingravitational-wavedetectors, Phys. Rev. D80, 084043 (2009), arXiv:0907.0700 [gr-qc]

    Pith/arXiv arXiv 2009

  53. [53]

    Hendriks, D

    K. Hendriks, D. Atallah, M. Martinez, M. Zevin, L. Zwick, A. A. Trani, P. Saini, J. Takátsy, and J. Samsing,Large Grav- itational Wave Phase Shifts from Strong 3-body Interactions in Dense Stellar Clusters, arXiv e-prints , arXiv:2411.08572 (2024), arXiv:2411.08572 [astro-ph.HE]

    arXiv 2024

  54. [54]

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

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

    Pith/arXiv arXiv 2021

  55. [55]

    C.García-Quirós,M.Colleoni,S.Husa,H.Estellés,G.Pratten, A.Ramos-Buades,M.Mateu-Lucena,andR.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]

    arXiv 2020

  56. [56]

    M.Hannam,P.Schmidt,A.Bohé,L.Haegel,S.Husa,F.Ohme, G.Pratten,andM.Pürrer,SimpleModelofCompletePrecessing Black-Hole-Binary Gravitational Waveforms, Phys. Rev. Lett. 113, 151101 (2014), arXiv:1308.3271 [gr-qc]

    Pith/arXiv arXiv 2014

  57. [57]

    LIGO Scientific Collaboration, LIGO Algorithm Library - LALSuite, free software (GPL) (2023)

    2023

  58. [58]

    Morras, G

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

    arXiv 2025

  59. [59]

    Klein,EFPE: Efficient fully precessing eccentric gravita- tionalwaveformsforbinarieswithlonginspirals,arXive-prints , arXiv:2106.10291 (2021), arXiv:2106.10291 [gr-qc]

    A. Klein,EFPE: Efficient fully precessing eccentric gravita- tionalwaveformsforbinarieswithlonginspirals,arXive-prints , arXiv:2106.10291 (2021), arXiv:2106.10291 [gr-qc]

    arXiv 2021

  60. [60]

    J.N.Arredondo,A.Klein,andN.Yunes,Efficientgravitational- wave model for fully-precessing and moderately eccentric, compact binary inspirals, Phys. Rev. D110, 044044 (2024), arXiv:2402.06804 [gr-qc]

    arXiv 2024

  61. [61]

    Damour and N

    T. Damour and N. Deruelle,General relativistic celestial me- chanics of binary systems. I. The post-newtonian motion, An- nales de l’I.H.P. Physique théorique43, 107–132 (1985)

    1985

  62. [62]

    Damour and N

    T. Damour and N. Deruelle,General relativistic celestial me- chanics of binary systems. II. The post-newtonian timing for- mula, Annales de l’I.H.P. Physique théorique44, 263–292 (1986)

    1986

  63. [63]

    Klein, N

    A. Klein, N. Cornish, and N. Yunes,Gravitational waveforms for precessing, quasicircular binaries via multiple scale anal- ysis and uniform asymptotics: The near spin alignment case, Phys. Rev. D88, 124015 (2013), arXiv:1305.1932 [gr-qc]

    Pith/arXiv arXiv 2013

  64. [64]

    Gerosa, G

    D. Gerosa, G. Fumagalli, M. Mould, G. Cavallotto, D. P. Mon- 16 roy, D. Gangardt, and V. De Renzis,Efficient multi-timescale dynamics of precessing black-hole binaries, Phys. Rev. D108, 024042 (2023), arXiv:2304.04801 [gr-qc]

    arXiv 2023

  65. [65]

    Klein, N

    A. Klein, N. Cornish, and N. Yunes,Fast Frequency-domain Waveforms for Spin-Precessing Binary Inspirals, Phys. Rev. D 90, 124029 (2014), arXiv:1408.5158 [gr-qc]

    Pith/arXiv arXiv 2014

  66. [66]

    R. J. E. Smith, G. Ashton, A. Vajpeyi, and C. Talbot,Massively parallelBayesianinferencefortransientgravitational-waveas- tronomy, Mon. Not. Roy. Astron. Soc.498, 4492–4502 (2020), arXiv:1909.11873 [gr-qc]

    arXiv 2020

  67. [67]

    Ashtonet al.,BILBY: A user-friendly Bayesian inference li- brary for gravitational-wave astronomy, Astrophys

    G. Ashtonet al.,BILBY: A user-friendly Bayesian inference li- brary for gravitational-wave astronomy, Astrophys. J. Suppl. 241, 27 (2019), arXiv:1811.02042 [astro-ph.IM]

    Pith/arXiv arXiv 2019

  68. [68]

    I. M. Romero-Shawet al.,Bayesian inference for compact binary coalescences with bilby: validation and application to the first LIGO–Virgo gravitational-wave transient cata- logue, Mon. Not. Roy. Astron. Soc.499, 3295–3319 (2020), arXiv:2006.00714 [astro-ph.IM]

    Pith/arXiv arXiv 2020

  69. [69]

    J. S. Speagle,dynesty: a dynamic nested sampling package for estimating Bayesian posteriors and evidences, Mon. Not. Roy. Astron. Soc.493, 3132–3158 (2020), arXiv:1904.02180 [astro- ph.IM]

    Pith/arXiv arXiv 2020

  70. [70]

    Skilling,Nested sampling for general Bayesian computation, Bayesian Analysis1, 833 – 859 (2006)

    J. Skilling,Nested sampling for general Bayesian computation, Bayesian Analysis1, 833 – 859 (2006)

    2006

  71. [71]

    Abbottet al.(LIGO Scientific, Virgo),GW190814: Gravi- tational Waves from the Coalescence of a 23 Solar Mass Black Holewitha2.6SolarMassCompactObject,Astrophys.J.Lett

    R. Abbottet al.(LIGO Scientific, Virgo),GW190814: Gravi- tational Waves from the Coalescence of a 23 Solar Mass Black Holewitha2.6SolarMassCompactObject,Astrophys.J.Lett. 896, L44 (2020), arXiv:2006.12611 [astro-ph.HE]

    Pith/arXiv arXiv 2020

  72. [72]

    S.Roy,A.S.Sengupta,andK.G.Arun,Unveilingthespectrum of inspiralling binary black holes, Phys. Rev. D103, 064012 (2021), arXiv:1910.04565 [gr-qc]

    arXiv 2021

  73. [73]

    L.Barsotti,S.Gras,M.Evans,andP.Fritschel,TheupdatedAd- vancedLIGOdesigncurve,LIGOTechnicalNoteT1800044-v5 (LIGOScientificCollaboration,2018)updatedfromT0900288- v3

    2018

  74. [74]

    Manzotti and A

    A. Manzotti and A. Dietz,Prospects for early localization of gravitational-wave signals from compact binary coalescences with advanced detectors, arXiv e-prints , arXiv:1202.4031 (2012), arXiv:1202.4031 [gr-qc]

    Pith/arXiv arXiv 2012

  75. [75]

    Abbottet al.(LIGO Scientific, KAGRA, VIRGO),Obser- vation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences, Astrophys

    R. Abbottet al.(LIGO Scientific, KAGRA, VIRGO),Obser- vation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences, Astrophys. J. Lett.915, L5 (2021), arXiv:2106.15163 [astro-ph.HE]

    arXiv 2021

  76. [76]

    Morras, G

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

    arXiv 2026

  77. [77]

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

    arXiv 2025

  78. [78]

    Kacanja, K

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

    arXiv 2025

  79. [79]

    A.Jan,B.-J.Tsao,R.O’Shaughnessy,D.Shoemaker,andP.La- guna,GW200105: A detailed study of eccentricity in the neu- tron star-black hole binary, Phys. Rev. D113, 024018 (2026), arXiv:2508.12460 [gr-qc]

    arXiv 2026

  80. [80]

    T. A. Clarke, I. M. Romero-Shaw, C. Hoy, J. Stegmann, P. D. Lasky, and E. Thrane,A universal framework to identify eccen- tric binary mergers: GW200105 case study, arXiv e-prints , arXiv:2605.18742 (2026), arXiv:2605.18742 [astro-ph.HE]

    Pith/arXiv arXiv 2026

Showing first 80 references.