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arxiv: 2606.31350 · v2 · pith:A5KZAPCSnew · submitted 2026-06-30 · 🌀 gr-qc

Compactness Inference in Gravitational-Wave Mergers with PhenomDECO: Catalog Benchmarks and Robustness Diagnostics

Shrobana Ghosh , Charlie Hoy , Mark Hannam , Frank Ohme This is my paper

Pith reviewed 2026-07-03 22:23 UTC · model grok-4.3

classification 🌀 gr-qc
keywords gravitational wavesbinary black holescompactness parameterGWTC-3 catalogwaveform modelslow-frequency noiseposterior analysisrobustness tests
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The pith

All high-significance GWTC-3 binary black hole candidates remain consistent with standard mergers once low-frequency noise is excluded.

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

The paper tests whether observed gravitational-wave signals from compact binaries match the expected shapes of binary black hole mergers by adding a single effective compactness parameter to an existing waveform model. In roughly 60 percent of events the posterior peaks near the expected value of 0.5, while about 20 percent show an extra low-compactness mode near 0.15 that vanishes when the analysis begins at higher frequencies, especially in the Livingston detector. Time-frequency residual comparisons after subtracting the best-fit waveforms confirm that the data are better explained by the standard model than by the deformed version in all cases examined. The work therefore supplies both a catalog benchmark and a practical diagnostic that low-frequency data handling must precede any claim of exotic compact-object physics.

Core claim

Applying PhenomDECO to every high-significance BBH event in GWTC-3 produces three recurring posterior shapes: near-Gaussian peaks at C approximately 0.5, additional high-compactness support above 0.8, and dominant low-compactness modes near C approximately 0.15. The low-compactness modes disappear when the data, particularly from Livingston, are reanalyzed from a higher starting frequency, indicating they arise from low-frequency noise artifacts rather than new physics. Residual checks after subtracting maximum-likelihood waveforms show that the data are better described by the baseline BBH model than by the compactness-deformed model. The study therefore concludes that all examined GWTC-3 o

What carries the argument

PhenomDECO, a phenomenological extension of a binary black hole waveform model that introduces a single effective compactness parameter C to quantify departures from standard merger morphology.

If this is right

  • Low-compactness modes seen in roughly 20 percent of events are eliminated by higher starting frequencies, showing they track low-frequency noise rather than source physics.
  • Time-frequency residuals after maximum-likelihood subtraction favor the standard BBH model over the compactness-deformed model in every case tested.
  • The method supplies a repeatable benchmark for future catalog analyses that must separate noise from possible deviations in merger morphology.
  • Low-frequency data treatment is required before any apparent departure from BBH expectations can be attributed to exotic sources.

Where Pith is reading between the lines

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

  • The same frequency-cut diagnostic could be applied routinely to high-mass events in upcoming observing runs to decide whether low-compactness modes warrant further investigation.
  • Joint multi-detector analysis above a common frequency threshold may become standard practice to avoid detector-specific noise mimicking non-standard compactness.
  • If the low-compactness modes are confirmed as noise, the approach strengthens the case that current detectors are not yet seeing exotic compact objects at merger.

Load-bearing premise

Raising the analysis starting frequency removes only noise artifacts without discarding genuine low-frequency signal content or biasing the compactness posterior.

What would settle it

A low-compactness posterior mode that survives when both detectors are analyzed above 50 Hz for GW231123, or a statistically significant improvement in time-frequency residuals when the PhenomDECO waveform is used instead of the baseline BBH waveform.

Figures

Figures reproduced from arXiv: 2606.31350 by Charlie Hoy, Frank Ohme, Mark Hannam, Shrobana Ghosh.

Figure 1
Figure 1. Figure 1: FIG. 1: The time domain GW signal associated with a BBH [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2: Frequency-domain amplitude for precessing binaries generated with the standard precessing binary waveform [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: Two-dimensional posterior probability distributions in mass ratio [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4: Time-domain [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5: The inferred e [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6: Plot showing the inferred compactness for events that show [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7: Plot showing the 2D marginalized posterior dis [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8: Compactness posterior distributions for the analyzed [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9: The lower panel shows the two-dimensional poste [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: FIG. 11: Posterior probability distributions for the total mass ( [PITH_FULL_IMAGE:figures/full_fig_p011_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: FIG. 12: Two-dimensional posterior distributions in total [PITH_FULL_IMAGE:figures/full_fig_p011_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: FIG. 13: Top left: spectrogram of the publicly available deglitched strain data for GW200129. Top right: residual spectrogram [PITH_FULL_IMAGE:figures/full_fig_p014_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: FIG. 14: Normalized energy distributions for two events. Left panel shows GW200219, which was identified in LVK tests of [PITH_FULL_IMAGE:figures/full_fig_p015_14.png] view at source ↗
read the original abstract

Several gravitational wave (GW) observations have been identified as binary black hole (BBH) mergers, including systems with component masses that challenge typical formation scenarios. These observations motivate broader tests of whether the detected sources are consistent with this interpretation. We address this question using~\deco~, an existing phenomenological extension of a BBH model that uses an effective compactness parameter to characterize departures from the expected merger morphology. Applying this model to all high-significance BBH events from GWTC-3, we establish~\deco~as a robust test of the nature of compact binaries. In preliminary analyses we identify three recurring posterior morphologies: (i) near-Gaussian peaks consistent with the BBH expectation $C\sim0.5$, seen in 60\% of events; (ii) posteriors with additional high-compactness support $(C\ge0.8)$; and (iii) dominant low-compactness modes near $C\sim0.15$ in $\sim 20\%$ of cases. For the latter, the low-compactness modes disappear when the data, especially from Livingston, are analyzed from a higher starting frequency, indicating sensitivity to low-frequency noise artefacts. We further use time--frequency residuals, computed after subtracting maximum-likelihood BBH and~\deco~waveforms from the strain data, to assess if the data is better described by a compactness-based deformation. With this analysis, we conclude that all of the GWTC-3 observations that we have considered are indeed consistent with BBH sources. The exception is the high-mass GW231123 signal, for which data from \emph{both} detectors must be analyzed above 50Hz to remove a low-compactness mode. This study shows that low-frequency data treatment is crucial before attributing apparent deviations from BBH expectations to exotic physics, and provides a benchmark for compactness-based tests of merger morphology in current and future GW detections.

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

2 major / 1 minor

Summary. The manuscript applies the PhenomDECO phenomenological model, extending a BBH waveform with an effective compactness parameter C, to high-significance GWTC-3 events. It identifies three posterior morphologies for C: near-Gaussian peaks at C~0.5 (60% of events), additional high-C support (C>=0.8), and dominant low-C modes at C~0.15 (~20% of cases). Low-C modes vanish when the analysis starting frequency is raised (especially Livingston data), which the authors attribute to low-frequency noise. Time-frequency residuals after subtracting maximum-likelihood BBH and PhenomDECO waveforms are used to assess model preference. The conclusion is that all considered GWTC-3 events are consistent with BBH sources except GW231123, which requires analysis above 50 Hz in both detectors.

Significance. If the frequency-cut tests and residual diagnostics are robust, the work supplies a useful catalog benchmark for compactness-based tests of merger morphology and underscores the necessity of careful low-frequency data treatment to avoid misinterpreting noise as exotic physics. The identification of recurring posterior patterns across the catalog provides a practical reference for future analyses of current and next-generation detectors.

major comments (2)
  1. [Abstract] Abstract (paragraph on low-compactness modes and Livingston data): The claim that low-C modes are noise artifacts (rather than new physics) rests on the premise that raising the starting frequency removes only artifacts without discarding genuine low-frequency signal content or biasing the C posterior. This premise is load-bearing for the final conclusion that all events are consistent with BBH sources, yet the manuscript provides no quantitative validation such as injected-signal recovery tests or explicit likelihood comparisons across frequency cuts.
  2. [Results on GW231123] Results on GW231123: The specific exception for GW231123 (requiring both detectors above 50 Hz) is presented without reported posterior comparisons, Bayes-factor changes, or justification for the exact 50 Hz threshold, making it difficult to evaluate whether the low-C mode removal is robust or an artifact of the cut choice.
minor comments (1)
  1. [Abstract] The abstract refers to 'preliminary analyses' for the three posterior morphologies; the main text should explicitly state whether these are the final reported results or a separate exploratory step.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful review and constructive comments on our manuscript. The points raised concern the robustness of our interpretation of low-compactness modes and the specific treatment of GW231123. We respond to each major comment below and indicate the revisions that will be incorporated.

read point-by-point responses

  1. Referee: [Abstract] Abstract (paragraph on low-compactness modes and Livingston data): The claim that low-C modes are noise artifacts (rather than new physics) rests on the premise that raising the starting frequency removes only artifacts without discarding genuine low-frequency signal content or biasing the C posterior. This premise is load-bearing for the final conclusion that all events are consistent with BBH sources, yet the manuscript provides no quantitative validation such as injected-signal recovery tests or explicit likelihood comparisons across frequency cuts.

    Authors: We acknowledge that the manuscript does not contain injected-signal recovery tests or explicit likelihood comparisons across frequency cuts. Our interpretation relies on the empirical, detector-specific disappearance of the low-C modes when the starting frequency is raised (particularly for Livingston data), combined with the time-frequency residual diagnostics. This pattern is reproducible across multiple events and aligns with known low-frequency noise characteristics. To address the concern directly, the revised manuscript will include explicit log-likelihood comparisons between the standard and higher-frequency analyses for a representative subset of events showing the low-C morphology. Full injection campaigns are outside the present scope but will be noted as a direction for follow-up work. revision: partial

  2. Referee: [Results on GW231123] Results on GW231123: The specific exception for GW231123 (requiring both detectors above 50 Hz) is presented without reported posterior comparisons, Bayes-factor changes, or justification for the exact 50 Hz threshold, making it difficult to evaluate whether the low-C mode removal is robust or an artifact of the cut choice.

    Authors: The 50 Hz threshold was selected after inspecting the evolution of the C posterior as the starting frequency was increased in 10 Hz steps; the low-C mode is suppressed once both detectors begin above this value. The revised manuscript will add the corresponding posterior distributions for C at multiple starting frequencies (20 Hz, 30 Hz, 40 Hz, 50 Hz) together with the change in maximum log-likelihood (or evidence) between the BBH and PhenomDECO models at each cut. This will allow quantitative assessment of the robustness of the chosen threshold. revision: yes

Circularity Check

0 steps flagged

No significant circularity; analysis is standard Bayesian application of pre-existing model

full rationale

The paper applies the existing PhenomDECO phenomenological model (with effective compactness parameter) to GWTC-3 strain data through Bayesian inference. Posterior morphologies (Gaussian peaks at C~0.5, high-C support, low-C modes at ~0.15) and their sensitivity to starting frequency are direct outputs of the sampling on the data. The conclusion that events are consistent with BBH sources (except GW231123) follows from these empirical posterior features without any step reducing by the paper's equations to a self-defined quantity, a fitted parameter renamed as prediction, or a load-bearing self-citation chain. No ansatz smuggling or renaming of known results is present; the frequency-cut interpretation is an interpretive assumption, not a definitional circularity.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on the validity of the PhenomDECO extension as a faithful representation of possible deviations and on the interpretation that low-compactness posterior modes are exclusively noise artifacts removable by frequency cuts.

free parameters (1)
  • effective compactness C
    Single phenomenological parameter introduced in the existing PhenomDECO model to capture departures from BBH merger morphology; its posterior is the main diagnostic quantity.
axioms (2)
  • domain assumption The PhenomDECO model extension accurately represents possible deviations from BBH merger morphology
    Invoked when using posterior support at C values away from 0.5 as evidence for or against exotic sources.
  • domain assumption Raising the analysis starting frequency removes only low-frequency noise without discarding genuine signal information
    Invoked when attributing disappearance of low-C modes to noise rather than new physics.

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Forward citations

Cited by 2 Pith papers

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

  1. Establishing Compactness as a Population Observable in Gravitational-Wave Astronomy

    gr-qc 2026-06 unverdicted novelty 5.0

    Hierarchical analysis of GWTC-3 events measures effective compactness C_eff = 0.5^{+0.3}_{-0.1} consistent with black holes and limits low-compactness exotic merger rate to <0.7 Gpc^{-3} yr^{-1}.

  2. Establishing Compactness as a Population Observable in Gravitational-Wave Astronomy

    gr-qc 2026-06 unverdicted novelty 4.0

    Hierarchical analysis of GWTC-3 yields C_eff = 0.5^{+0.3}_{-0.1} consistent with black holes and limits low-compactness exotic binary merger rate to <0.7 Gpc^{-3} yr^{-1}.

Reference graph

Works this paper leans on

86 extracted references · 86 canonical work pages · cited by 1 Pith paper · 42 internal anchors

  1. [1]

    Dominant peak near C=0.5 About two thirds of the events show posteriors consistent with BBH, which we classify as typical behaviour. As shown in Figure 6, this category includes posteriors that: (i) exhibit a clear peak near C =0 .5 (GW190731); (ii) peak at 0.5, but with a very broad 90% credible interval (CI) (GW170608); (iii) are bimodal, with peaks dis...

    work page

  2. [2]

    Only one event shows a clear preference for C∼ 0.9 (GW170818), and in two other events C =0 .5 is excluded at 90% lower CI

    Support for C>0.5 We found significant support for a compactness much higher than 0.5 for about ten events. Only one event shows a clear preference for C∼ 0.9 (GW170818), and in two other events C =0 .5 is excluded at 90% lower CI. In all the other cases, although the posterior probability favours a higher compactness, C =0 .5 was always included in the 9...

    work page

  3. [3]

    However, as discussed above, modest downward deviations from 0.5 can arise for a variety of non- exotic reasons

    Spuriously low measure of compactness Nominally, a compactness posterior whose upper 90% CI lies below 0.5 would suggest that one or both components are of exotic origin. However, as discussed above, modest downward deviations from 0.5 can arise for a variety of non- exotic reasons. We therefore regard a compactness posterior as potentially suggestive of ...

    work page

  4. [4]

    This event is the most mas- sive BBH system observed to date by the LVK and was detected by the LIGO Livingston and Hanford observatories

    Event properties and analysis challenges We consider here the inference of source properties of GW231123 with PhenomDECO. This event is the most mas- sive BBH system observed to date by the LVK and was detected by the LIGO Livingston and Hanford observatories. Because of the binary’s short in-band duration, the detected signal is dominated by the merger-r...

    work page

  5. [5]

    10: Effective compactness inference for GW231123 using data above 20 Hz in both Livingston and Hanford is shown in blue

    Effective compactness inference 0.1 0.2 0.3 0.4 0.5 0.6 Effective compactness H1-20 L1-20 H1-20 L1-50 H1-50 L1-20 H1-50 L1-50 FIG. 10: Effective compactness inference for GW231123 using data above 20 Hz in both Livingston and Hanford is shown in blue. Raising the low-frequency cutoffto 50 Hz in either detector, while keeping the other at 20 Hz, leaves the ...

    work page

  6. [6]

    Ordinarily, the persistence of a low-compactness mode under single- detector cutofftests would make the event more suggestive of genuine non-BBH structure

    Interpretation Within our analysis, GW231123 stands out as a special case in that a BBH-like characterization with PhenomDECO is obtained only after raising the low- frequency cutoffconsistently in both detectors. Ordinarily, the persistence of a low-compactness mode under single- detector cutofftests would make the event more suggestive of genuine non-BB...

    work page

  7. [7]

    Using a low frequency cutoffof 50 Hz for Livingston data, while keeping 20 Hz for Hanford, shifts the recovered com- pactness posterior to a peak near 0.5

    GW200129 First, we consider GW200129 which is one of the events where we found a spurious low-compactness peak at ∼ 0.15. Using a low frequency cutoffof 50 Hz for Livingston data, while keeping 20 Hz for Hanford, shifts the recovered com- pactness posterior to a peak near 0.5. The associated spec- trograms are consistent with this behaviour: the maximum- ...

    work page

  8. [8]

    This is comparable to what we find for events in which the likelihood peaks near C∼ 0.5 (see Table I)

    GW191127 We then consider GW191127 and find the likeli- hood function to peak for a compactness C∼ 0.35 (logLC=0.5 =33 .69 and logLC=0.35 =48 .06 ) in Bayesian analysis, with a residual contrast of 0.037 be- tween PhenomDECO and PhenomXPHM . This is comparable to what we find for events in which the likelihood peaks near C∼ 0.5 (see Table I). Taken in iso...

    work page

  9. [9]

    13: Top left: spectrogram of the publicly available deglitched strain data for GW200129

    GW200219 Finally, we consider GW200219, which was reported with the largest residual SNR and, more importantly, the 14 FIG. 13: Top left: spectrogram of the publicly available deglitched strain data for GW200129. Top right: residual spectrogram obtained after subtracting the maximum-likelihood PhenomDECO waveform from the analysis that favors C∼ 0.15. Bot...

    work page

  10. [11]

    A. H. Nitz, S. Kumar, Y .-F. Wang, S. Kastha, S. Wu, M. Schäfer, R. Dhurkunde, and C. D. Capano, 4-ogc: Catalog of gravitational waves from compact binary mergers, The Astrophysical Journal946, 59 (2023)

    work page 2023

  11. [12]

    Venumadhav, B

    T. Venumadhav, B. Zackay, J. Roulet, L. Dai, and M. Zaldar- riaga, New binary black hole mergers in the second observing run of advanced ligo and advanced virgo, Phys. Rev. D101, 083030 (2020)

    work page 2020

  12. [13]

    Olsen, T

    S. Olsen, T. Venumadhav, J. Mushkin, J. Roulet, B. Zackay, and M. Zaldarriaga, New binary black hole mergers in the LIGO-Virgo O3a data, Phys. Rev. D106, 043009 (2022), arXiv:2201.02252 [astro-ph.HE]

    work page arXiv 2022

  13. [14]

    A. K. Mehta, S. Olsen, D. Wadekar, J. Roulet, T. Venumadhav, J. Mushkin, B. Zackay, and M. Zaldarriaga, New binary black hole mergers in the LIGO-Virgo O3b data, Phys. Rev. D111, 024049 (2025), arXiv:2311.06061 [gr-qc]

    work page arXiv 2025

  14. [15]

    A. G. Abacet al.(LIGO Scientific Collaboration and Virgo Collaboration and KAGRA Collaboration), GWTC-4.0: Up- dating the gravitational-wave transient catalog with ob- servations from the first part of the fourth LIGO-Virgo- KAGRA observing run 10.48550/arXiv.2508.18082 (2025), arXiv:2508.18082 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2508.18082 2025

  15. [16]

    GWTC-5.0: An Introduction to Version 5.0 of the Gravitational-Wave Transient Catalog

    N. Abacet al.(LIGO Scientific, VIRGO, KAGRA), GWTC- 5.0: An Introduction to Version 5.0 of the Gravitational-Wave Transient Catalog, (2026), arXiv:2605.27223 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  16. [17]

    GWTC-5.0: Population Properties of Merging Compact Bi- naries, (2026), arXiv:2605.27226 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  17. [18]

    R. Abbottet al.(LIGO Scientific Collaboration and Virgo Collaboration), GW190814: Gravitational waves from the coalescence of a 23 solar mass black hole with a 2.6 solar mass compact object, The Astrophysical Journal Letters896, L44 (2020), arXiv:2006.12611 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  18. [19]

    A. G. Abacet al.(LIGO Scientific Collaboration and Virgo Collaboration and KAGRA Collaboration), Observation of gravitational waves from the coalescence of a 2 .5–4.5 m⊙ compact object and a neutron star, The Astrophysical Journal Letters970, L34 (2024), arXiv:2404.04248 [astro-ph.HE]

    work page arXiv 2024

  19. [20]

    R. Abbottet al.(LIGO Scientific Collaboration and Virgo Collaboration), GW190521: A binary black hole merger with a total mass of 150 m⊙, Physical Review Letters125, 101102 (2020), arXiv:2009.01075 [gr-qc]. 18

    work page arXiv 2020

  20. [21]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), GW231123: A Binary Black Hole Merger with Total Mass 190–265 M ⊙, Astrophys. J. Lett.993, L25 (2025), arXiv:2507.08219 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  21. [22]

    Phenomenological template family for black-hole coalescence waveforms

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

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  22. [23]

    Inspiral-merger-ringdown waveforms for black-hole binaries with non-precessing spins

    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]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  23. [24]

    S. Khan, S. Husa, M. Hannam, F. Ohme, M. Pürrer, X. Jiménez Forteza, and A. Bohé, Frequency-domain gravi- tational waves from nonprecessing black-hole binaries. II. A phenomenological model for the advanced detector era, Phys. Rev. D93, 044007 (2016), arXiv:1508.07253 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  24. [25]

    S. Husa, S. Khan, M. Hannam, M. Pürrer, F. Ohme, X. Jiménez Forteza, and A. Bohé, Frequency-domain gravita- tional waves from nonprecessing black-hole binaries. I. New numerical waveforms and anatomy of the signal, Phys. Rev. D93, 044006 (2016), arXiv:1508.07250 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  25. [26]

    A simple model of complete precessing black-hole-binary gravitational waveforms

    M. Hannam, P. Schmidt, A. Bohé, L. Haegel, S. Husa, F. Ohme, G. Pratten, and M. Pürrer, Simple Model of Complete Precessing Black-Hole-Binary Gravitational Wave- forms, Phys. Rev. Lett.113, 151101 (2014), arXiv:1308.3271 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  26. [27]

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

    work page arXiv 2024

  27. [28]

    Colleoni, F

    M. Colleoni, F. A. R. Vidal, C. García-Quirós, S. Akçay, and S. Bera, Fast frequency-domain gravitational waveforms for precessing binaries with a new twist, Phys. Rev. D111, 104019 (2025), arXiv:2412.16721 [gr-qc]

    work page arXiv 2025

  28. [29]

    Hamiltonet al., Improved gravitational wave model link- ing precessing inspirals and numerical-relativity-calibrated merger-ringdown, Phys

    E. Hamiltonet al., Improved gravitational wave model link- ing precessing inspirals and numerical-relativity-calibrated merger-ringdown, Phys. Rev. D113, 084055 (2026), arXiv:2507.02604 [gr-qc]

    work page arXiv 2026

  29. [30]

    Ghosh, P

    S. Ghosh, P. Kolitsidou, and M. Hannam, First frequency- domain phenomenological model of the multipole asymmetry in gravitational-wave signals from binary-black-hole coales- cence, Phys. Rev. D109, 024061 (2024), arXiv:2310.16980 [gr-qc]

    work page arXiv 2024

  30. [31]

    Effective one-body approach to general relativistic two-body dynamics

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

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  31. [32]

    Transition from inspiral to plunge in binary black hole coalescences

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

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  32. [33]

    Effective-one-body model for black-hole binaries with generic mass ratios and spins

    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]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  33. [34]

    Transition from inspiral to plunge in precessing binaries of spinning black holes

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

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  34. [35]

    Ramos-Buades, A

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

    work page arXiv 2023

  35. [36]

    Estellés, A

    H. Estellés, A. Buonanno, R. Enficiaud, C. Foo, and L. Pom- pili, Adding equatorial-asymmetric effects for spin-precessing binaries into the seobnrv5phm waveform model, Phys. Rev. D113, 044049 (2026), arXiv:2506.19911 [gr-qc]

    work page arXiv 2026

  36. [37]

    Evstafyeva, U

    T. Evstafyeva, U. Sperhake, I. Romero-Shaw, and M. Agathos, Gravitational-wave data analysis with high-precision numer- ical relativity simulations of boson star mergers, (2024), arXiv:2406.02715 [gr-qc]

    work page arXiv 2024

  37. [38]

    Lessons from binary dynamics of inspiralling equal-mass boson-star mergers

    T. Evstafyeva, A. Seifert, U. Sperhake, C. J. Moore, and T. Jain, Lessons from binary dynamics of inspiralling equal- mass boson-star mergers, (2026), arXiv:2604.25582 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  38. [39]

    Tests of General Relativity with GWTC-3

    R. Abbottet al.(LIGO Scientific, VIRGO, KAGRA), Tests of General Relativity with GWTC-3, Phys. Rev. D112, 084080 (2025), arXiv:2112.06861 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  39. [40]

    Ghosh and M

    S. Ghosh and M. Hannam, Identification of exotic compact binaries with gravitational waves: A phenomenological ap- proach, Phys. Rev. D112, 104017 (2025), arXiv:2505.16380 [gr-qc]

    work page arXiv 2025

  40. [41]

    Establishing Compactness as a Population Observable in Gravitational-Wave Astronomy

    S. Ghosh, C. Hoy, M. Hannam, and F. Ohme, Establishing Compactness as a Population Observable in Gravitational- Wave Astronomy, (2026), arXiv:2606.31364 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  41. [42]

    Advanced LIGO

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

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  42. [43]

    Buikemaet al.(aLIGO), Sensitivity and performance of the Advanced LIGO detectors in the third observing run, Phys

    A. Buikemaet al.(aLIGO), Sensitivity and performance of the Advanced LIGO detectors in the third observing run, Phys. Rev. D102, 062003 (2020), arXiv:2008.01301 [astro-ph.IM]

    work page arXiv 2020

  43. [44]

    Tseet al., Quantum-Enhanced Advanced LIGO Detectors in the Era of Gravitational-Wave Astronomy, Phys

    M. Tseet al., Quantum-Enhanced Advanced LIGO Detectors in the Era of Gravitational-Wave Astronomy, Phys. Rev. Lett. 123, 231107 (2019)

    work page 2019

  44. [45]

    Advanced Virgo: a 2nd generation interferometric gravitational wave detector

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

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  45. [46]

    Acerneseet al.(Virgo), Increasing the Astrophysical Reach of the Advanced Virgo Detector via the Application of Squeezed Vacuum States of Light, Phys

    F. Acerneseet al.(Virgo), Increasing the Astrophysical Reach of the Advanced Virgo Detector via the Application of Squeezed Vacuum States of Light, Phys. Rev. Lett.123, 231108 (2019)

    work page 2019

  46. [47]

    Acerneseet al.(Virgo), Virgo detector characteriza- tion and data quality: results from the O3 run, Class

    F. Acerneseet al.(Virgo), Virgo detector characterization and data quality: results from the O3 run, Class. Quant. Grav.40, 185006 (2023), arXiv:2210.15633 [gr-qc]

    work page arXiv 2023

  47. [48]

    Somiya (KAGRA), Class

    K. Somiya (KAGRA), Detector configuration of KAGRA: The Japanese cryogenic gravitational-wave detector, Class. Quant. Grav.29, 124007 (2012), arXiv:1111.7185 [gr-qc]

    work page arXiv 2012

  48. [49]

    Y . Aso, Y . Michimura, K. Somiya, M. Ando, O. Miyakawa, T. Sekiguchi, D. Tatsumi, and H. Yamamoto (The KAGRA Collaboration), Interferometer design of the kagra gravita- tional wave detector, Phys. Rev. D88, 043007 (2013)

    work page 2013

  49. [50]

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

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

    work page arXiv 2021

  50. [51]

    N. V . Krishnendu, K. G. Arun, and C. K. Mishra, Testing the binary black hole nature of a compact binary coalescence, Phys. Rev. Lett.119, 091101 (2017), arXiv:1701.06318 [gr- qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  51. [52]

    N. V . Krishnendu, M. Saleem, A. Samajdar, K. G. Arun, W. Del Pozzo, and C. K. Mishra, Constraints on the binary black hole nature of GW151226 and GW170608 from the measurement of spin-induced quadrupole moments, Phys. Rev. D100, 104019 (2019), arXiv:1908.02247 [gr-qc]

    work page arXiv 2019

  52. [53]

    N. V . Krishnendu, F. Ohme, and K. G. Arun, Testing the nature of compact objects in the lower mass gap using gravi- tational wave observations (2025), arXiv:2509.10420 [astro- ph.HE]

    work page arXiv 2025

  53. [54]

    Black Hole Spectroscopy: Testing General Relativity through Gravitational Wave Observations

    O. Dreyer, B. J. Kelly, B. Krishnan, L. S. Finn, D. Garrison, and R. Lopez-Aleman, Black hole spectroscopy: Testing general relativity through gravitational wave observations, Class. Quant. Grav.21, 787 (2004), arXiv:gr-qc/0309007

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  54. [55]

    Berti, V

    E. Berti, V . Cardoso, and C. M. Will, On gravitational-wave spectroscopy of massive black holes with the space inter- ferometer LISA, Phys. Rev. D73, 064030 (2006), arXiv:gr- qc/0512160

    work page arXiv 2006

  55. [56]

    Uchikata, H

    N. Uchikata, H. Nakano, T. Narikawa, N. Sago, H. Tagoshi, and T. Tanaka, Searching for black hole echoes from the LIGO-Virgo Catalog GWTC-1, Phys. Rev. D100, 062006 (2019), arXiv:1906.00838 [gr-qc]. 19

    work page arXiv 2019

  56. [57]

    Uchikata, T

    N. Uchikata, T. Narikawa, H. Nakano, N. Sago, H. Tagoshi, and T. Tanaka, Searching for gravitational wave echoes from black hole binary events in the third observing run of LIGO, Virgo, and KAGRA collaborations, Phys. Rev. D108, 104040 (2023), arXiv:2309.01894 [gr-qc]

    work page arXiv 2023

  57. [58]

    S. A. Hughes and K. Menou, Golden binaries for LISA: Ro- bust probes of strong-field gravity, Astrophys. J.623, 689 (2005), arXiv:astro-ph/0410148

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  58. [59]

    Testing general relativity using golden black-hole binaries

    A. Ghoshet al., Testing general relativity using golden black-hole binaries, Phys. Rev. D94, 021101 (2016), arXiv:1602.02453 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  59. [60]

    Head-on collisions of boson stars

    C. Palenzuela, I. Olabarrieta, L. Lehner, and S. L. Liebling, Head-on collisions of boson stars, Phys. Rev. D75, 064005 (2007), arXiv:gr-qc/0612067

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  60. [61]

    Orbital Dynamics of Binary Boson Star Systems

    C. Palenzuela, L. Lehner, and S. L. Liebling, Orbital Dynam- ics of Binary Boson Star Systems, Phys. Rev. D77, 044036 (2008), arXiv:0706.2435 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  61. [62]

    Full 3D Numerical Relativity Simulations of Neutron Star -- Boson Star Collisions with BAM

    T. Dietrich, S. Ossokine, and K. Clough, Full 3D numer- ical relativity simulations of neutron star–boson star colli- sions with BAM, Class. Quant. Grav.36, 025002 (2019), arXiv:1807.06959 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  62. [63]

    Axion star collisions with black holes and neutron stars in full 3D numerical relativity

    K. Clough, T. Dietrich, and J. C. Niemeyer, Axion star colli- sions with black holes and neutron stars in full 3D numerical relativity, Phys. Rev. D98, 083020 (2018), arXiv:1808.04668 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  63. [64]

    Siemonsen and W

    N. Siemonsen and W. E. East, Binary boson stars: Merger dynamics and formation of rotating remnant stars, Phys. Rev. D107, 124018 (2023), arXiv:2302.06627 [gr-qc]

    work page arXiv 2023

  64. [65]

    Computationally efficient models for the dominant and sub-dominant harmonic modes of precessing binary black holes

    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]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  65. [66]

    Sensitivity Studies for Third-Generation Gravitational Wave Observatories

    S. Hildet al., Sensitivity Studies for Third-Generation Gravi- tational Wave Observatories, Class. Quant. Grav.28, 094013 (2011), arXiv:1012.0908 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  66. [67]

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

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  67. [68]

    Bilby: A user-friendly Bayesian inference library for gravitational-wave astronomy

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

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  68. [69]

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

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  69. [70]

    CoRe database of binary neutron star merger waveforms and its application in waveform development

    T. Dietrich, D. Radice, S. Bernuzzi, F. Zappa, A. Perego, B. Brügmann, S. V . Chaurasia, R. Dudi, W. Tichy, and M. Uje- vic, CoRe database of binary neutron star merger waveforms, Class. Quant. Grav.35, 24LT01 (2018), arXiv:1806.01625 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  70. [71]

    R. Dudi, F. Pannarale, T. Dietrich, M. Hannam, S. Bernuzzi, F. Ohme, and B. Brügmann, Relevance of tidal effects and post-merger dynamics for binary neutron star parameter esti- mation, Phys. Rev. D98, 084061 (2018), arXiv:1808.09749 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  71. [72]

    Hannamet al., General-relativistic precession in a black- hole binary, Nature610, 652 (2022), arXiv:2112.11300 [gr- qc]

    M. Hannamet al., General-relativistic precession in a black- hole binary, Nature610, 652 (2022), arXiv:2112.11300 [gr- qc]

    work page arXiv 2022

  72. [73]

    Payne, S

    E. Payne, S. Hourihane, J. Golomb, R. Udall, R. Udall, D. Davis, and K. Chatziioannou, Curious case of GW200129: Interplay between spin-precession inference and data-quality issues, Phys. Rev. D106, 104017 (2022), arXiv:2206.11932 [gr-qc]

    work page arXiv 2022

  73. [74]

    Scattered light noise at LIGO Livingston Observatory during O4

    D. Nandi, A. Effler, S. Soni, T. A. Ferreira, R. Schofield, H. Pham, T. O’Hanlon, V . V . Frolov, and G. González, Scat- tered light noise at ligo livingston observatory during o4 (2026), arXiv:2605.14143 [astro-ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  74. [75]

    A. G. Abacet al.(LIGO Scientific, Virgo, KAGRA), GW250114: Testing Hawking’s Area Law and the Kerr Na- ture of Black Holes, Phys. Rev. Lett.135, 111403 (2025), arXiv:2509.08054 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  75. [76]

    Abbott et al

    R. Abbottet al.(LIGO Scientific, Virgo), GW190412: Obser- vation of a Binary-Black-Hole Coalescence with Asymmetric Masses, Phys. Rev. D102, 043015 (2020), arXiv:2004.08342 [astro-ph.HE]

    work page arXiv 2020

  76. [77]

    A. G. Abacet al.(LIGO Scientific, Virgo, KAGRA), Black Hole Spectroscopy and Tests of General Relativ- ity with GW250114, Phys. Rev. Lett.136, 041403 (2026), arXiv:2509.08099 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  77. [78]

    Akyüz, A

    A. Akyüz, A. Correia, J. Garofalo, K. Kacanja, L. Roy, K. Soni, H. Tan, V . J. Y , A. H. Nitz, and C. D. Capano, Poten- tial science with GW250114 – the loudest binary black hole merger detected to date, (2025), arXiv:2507.08789 [gr-qc]

    work page arXiv 2025

  78. [79]

    Plunge-Merger-Ringdown Tests of General Relativity with GW250114

    L. Grimaldi, E. Maggio, L. Pompili, and A. Buo- nanno, Plunge-merger-ringdown tests of general relativ- ity with GW250114, Phys. Rev. D113, L061506 (2026), arXiv:2601.13173 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  79. [80]

    S. Bini, K. Król, K. Chatziioannou, and M. Isi, The impact of waveform systematics and Gaussian noise on the interpreta- tion of GW231123, (2026), arXiv:2601.09678 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  80. [81]

    Dideron, S

    G. Dideron, S. Mukherjee, and L. Lehner, SCoRe: A New Framework to Study Unmodeled Physics from Grav- itational Wave Data, Phys. Rev. D107, 104023 (2023), arXiv:2209.14321 [gr-qc]

    work page arXiv 2023

Showing first 80 references.