Recognition: no theorem link
GW250114: testing Hawking's area law and the Kerr nature of black holes
Pith reviewed 2026-05-13 21:23 UTC · model grok-4.3
The pith
GW250114 data confirm the final black hole area exceeds the sum of the two progenitors and its ringdown matches a Kerr spectrum.
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
Core claim
Post-merger data excluding the peak region are consistent with the dominant quadrupolar mode of a Kerr black hole and its first overtone, with frequencies constrained to plus or minus thirty percent of the Kerr spectrum. Analyses that exclude up to five of the strongest merger cycles show the remnant area is larger than the sum of the initial areas to high credibility.
What carries the argument
Matched-filter comparison of post-peak waveform segments to Kerr quasinormal-mode templates together with direct area computation from inferred initial and final masses and spins.
Load-bearing premise
The full waveform from inspiral through ringdown is assumed to be accurately described by general-relativity templates that presuppose a Kerr remnant.
What would settle it
An observation in which the inferred remnant area falls below the sum of the initial areas, or in which the measured ringdown frequencies lie more than thirty percent away from the Kerr values, would contradict the reported result.
read the original abstract
The gravitational-wave signal GW250114 was observed by the two LIGO detectors with a network matched-filter signal-to-noise ratio of 80. The signal was emitted by the coalescence of two black holes with near-equal masses $m_1 = 33.6^{+1.2}_{-0.8}\,M_\odot$ and $m_2 = 32.2^{+0.8}_{-1.3}\,M_\odot$, and small spins $\chi_{1,2} \leq 0.26$ (90% credibility) and negligible eccentricity $e \leq 0.03$. Post-merger data excluding the peak region are consistent with the dominant quadrupolar $(\ell = |m| = 2)$ mode of a Kerr black hole and its first overtone. We constrain the modes' frequencies to $\pm 30\%$ of the Kerr spectrum, providing a test of the remnant's Kerr nature. We also examine Hawking's area law, also known as the second law of black hole mechanics, which states that the total area of the black hole event horizons cannot decrease with time. A range of analyses that exclude up to 5 of the strongest merger cycles confirm that the remnant area is larger than the sum of the initial areas to high credibility.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper analyzes the high-SNR LIGO event GW250114 from the merger of two near-equal-mass black holes (m1 ≈ 33.6 M⊙, m2 ≈ 32.2 M⊙, low spins). Using post-merger data with the peak excised, it reports consistency with the dominant (ℓ=|m|=2) quadrupolar mode and first overtone of a Kerr remnant, constraining the frequencies to within ±30% of the Kerr spectrum. Multiple analyses excluding up to five strong merger cycles show the remnant horizon area exceeds the sum of the initial areas at high credibility, supporting Hawking's area law.
Significance. If the results hold, the work supplies one of the cleanest observational consistency checks of the black-hole area theorem and the no-hair property of the remnant using real gravitational-wave data. The deliberate excision of the loudest cycles and the use of established LIGO parameter-estimation pipelines are strengths that reduce contamination from the merger phase. The reported credibility intervals on the area increase and the frequency bound constitute falsifiable, data-driven statements that can be directly compared with future events.
major comments (2)
- [Parameter estimation and ringdown analysis sections] The parameter-estimation step that supplies both the initial areas (from inspiral) and the remnant mass/spin (from ringdown) is performed exclusively with GR waveform templates that already assume a Kerr remnant. Any unmodeled systematic mismatch between these templates and the true signal therefore propagates directly into the reported ±30% frequency bound and the A_remnant > A1 + A2 credibility. The robustness tests vary only the data segment length; they do not vary the template family or relax the Kerr assumption.
- [Post-merger frequency constraint paragraph] The ±30% frequency constraint is presented as a test of the Kerr nature, yet the bound is derived after the remnant parameters have already been inferred under the Kerr hypothesis. It is therefore a consistency check rather than an independent measurement; the manuscript should quantify how much the bound would loosen if the remnant spin were allowed to float freely or if a non-Kerr ringdown model were substituted.
minor comments (2)
- [Abstract and results section] The abstract states that 'a range of analyses' exclude up to five cycles; the main text should list the exact set of excision windows and the corresponding credibility values for the area increase so that readers can reproduce the robustness claim.
- [Introduction and methods] Notation for the initial and remnant areas (A1, A2, A_remnant) should be defined explicitly the first time they appear, including the precise formula used to compute horizon area from mass and spin.
Simulated Author's Rebuttal
We thank the referee for the positive assessment and constructive comments on our analysis of GW250114. We have revised the manuscript to clarify the assumptions in our parameter estimation and to describe the frequency constraint explicitly as a consistency check. Below we respond point by point to the major comments.
read point-by-point responses
-
Referee: [Parameter estimation and ringdown analysis sections] The parameter-estimation step that supplies both the initial areas (from inspiral) and the remnant mass/spin (from ringdown) is performed exclusively with GR waveform templates that already assume a Kerr remnant. Any unmodeled systematic mismatch between these templates and the true signal therefore propagates directly into the reported ±30% frequency bound and the A_remnant > A1 + A2 credibility. The robustness tests vary only the data segment length; they do not vary the template family or relax the Kerr assumption.
Authors: We agree that the analysis relies on standard GR waveform templates (such as IMRPhenomXPHM) that assume a Kerr remnant, which is the established approach for LIGO parameter estimation of this event. The robustness tests were designed to assess the impact of including or excluding merger cycles, the main potential source of bias in the ringdown regime. While we did not vary template families or relax the Kerr assumption, these templates have been extensively validated against numerical relativity for systems with mass ratios and spins comparable to GW250114. We have added clarifying text in the revised manuscript stating that the reported bounds are conditional on the GR templates and discussing possible systematic effects. This constitutes a partial revision, as we incorporated discussion but did not conduct new template-variation studies. revision: partial
-
Referee: [Post-merger frequency constraint paragraph] The ±30% frequency constraint is presented as a test of the Kerr nature, yet the bound is derived after the remnant parameters have already been inferred under the Kerr hypothesis. It is therefore a consistency check rather than an independent measurement; the manuscript should quantify how much the bound would loosen if the remnant spin were allowed to float freely or if a non-Kerr ringdown model were substituted.
Authors: We acknowledge that the ±30% frequency bound is a consistency check performed after inferring remnant parameters under the Kerr hypothesis. We have revised the relevant paragraph to describe the result explicitly as a consistency test within the GR framework rather than an independent measurement. A full quantification of how the bound would change under a freely floating spin or a non-Kerr ringdown model would require implementing alternative models outside the standard LIGO pipelines, which lies beyond the scope of this work. We have added a note in the discussion section highlighting this limitation and identifying it as a direction for future analyses. revision: partial
Circularity Check
No significant circularity in derivation chain
full rationale
The paper infers initial and remnant parameters via standard GR waveform templates, then performs consistency checks by comparing post-merger frequencies to the external Kerr spectrum (computed from inferred mass/spin) and verifying that the remnant area exceeds the sum of initial areas using the GR area formula. These are external theoretical benchmarks, not quantities fitted or defined from the same data segment in a self-referential loop. No self-definitional equations, fitted inputs relabeled as predictions, load-bearing self-citations, or ansatzes smuggled via prior work appear in the described chain. The tests remain independent consistency checks against GR theory even when merger cycles are excised.
Axiom & Free-Parameter Ledger
free parameters (1)
- component masses and spins
axioms (2)
- domain assumption The spacetime of the remnant is exactly described by the Kerr metric
- domain assumption Hawking's area theorem applies to the classical event horizons inferred from the data
Forward citations
Cited by 22 Pith papers
-
GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors
The first informative astrophysical calibration of gravitational-wave detectors is reported using GW240925 and GW250207.
-
Black-Hole Scattering in Einstein-scalar-Gauss-Bonnet: Numerical Relativity Meets Analytics
Numerical relativity simulations of black hole scattering in Einstein-scalar-Gauss-Bonnet gravity agree closely with effective-one-body analytic predictions.
-
Testing the Kerr hypothesis beyond the quadrupole with GW241011
GW241011 data shows consistency with Kerr black holes for both quadrupole and octupole moments and delivers the first observational bounds on spin-induced octupole deviations.
-
Resonances as signatures of scalar clouds in eccentric extreme-mass-ratio inspirals
Eccentricity in EMRIs around scalar clouds produces relativistic resonances in scalar fluxes near the last stable orbit, leading to observable dephasing in gravitational waveforms.
-
Lessons from binary dynamics of inspiralling equal-mass boson-star mergers
Numerical simulations of equal-mass boson-star mergers reveal larger waveform deviations from black-hole binaries in late inspiral and merger, plus odd multipole excitations for certain scalar-field phases, with some ...
-
How lonely are the Binary Compact Objects Detected by the LIGO-Virgo-KAGRA Collaboration?
No three-body encounter signatures detected in GW170817, GW190814, and GW230627_015337, constraining intermediate-mass black holes above 100 solar masses within roughly 0.1 AU of these binaries.
-
Highly eccentric non-spinning binary black hole mergers: quadrupolar post-merger waveforms
Polynomial models for the (2,2) post-merger waveform amplitudes of eccentric non-spinning binary black holes are constructed from numerical-relativity data as functions of symmetric mass ratio and two merger-time dyna...
-
Novel ringdown tests of general relativity with black hole greybody factors
GreyRing model based on greybody factors reproduces numerical relativity ringdown signals with mismatches of order 10^{-6} and enables a new post-merger consistency test of general relativity applied to GW250114.
-
Quadratic gravity corrections to scalar QNMs of rapidly rotating black holes
Leading-order deviations from general relativity in scalar quasinormal modes of rotating black holes are computed numerically up to dimensionless spins of 0.99 in quadratic-curvature scalar-tensor theories.
-
Accelerated Time-domain Analysis for Gravitational Wave Astronomy
Presents a practical fully time-domain end-to-end likelihood for gravitational-wave inference with structured linear algebra and GPU acceleration.
-
Cracking Gravitational Wave Multiple Ringdown Modes in Space
FIREFLY algorithm enables 200-fold faster multi-mode ringdown analysis for space-borne gravitational wave detectors while remaining compatible with time-delay interferometry.
-
Fast neural network surrogate for multimodal effective-one-body gravitational waveforms from generically precessing compact binaries
Neural network surrogate approximates precessing compact binary gravitational waveforms up to 1000x faster than the base EOB model with validated accuracy.
-
All-order structure of static gravitational interactions and the seventh post-Newtonian potential
A closed formula computes static post-Newtonian corrections at arbitrary odd orders in gravity, yielding the explicit seventh post-Newtonian potential that matches an independent diagrammatic method.
-
Ringing of rapidly rotating black holes in effective field theory
Leading-order cubic-curvature corrections to scalar quasinormal modes of black holes with spins up to 0.99M are computed numerically for modes up to l=5 with relative errors below 10^{-4}.
-
Ringdown Analysis of GW250114 with Orthonormal Modes
Orthonormal QNM analysis of GW250114 raises the significance of the first overtone of the ℓ=m=2 mode from 82.5% to 99.9% and detects no significant deviation from Kerr predictions.
-
The properties and predictions of quasi-periodic oscillations around a black hole in nonlocal gravity
Nonlocal gravity shrinks the ISCO radius, boosts QPO frequencies, and constrains α/M ≤ 0.452 with M ≲ 43.6 M_⊙ for observed high-frequency QPOs under resonance models.
-
Hawking area law in quantum gravity
Exact Hawking area law from black hole mergers restricts quantum gravity to singular Ricci-flat or specific regular black holes in Stelle and nonlocal theories, derives the standard entropy-area law, and realizes Barr...
-
Probing Kerr Symmetry Breaking with LISA Extreme-Mass-Ratio Inspirals
LISA EMRIs can constrain deviations from Kerr equatorial symmetry to 10^{-2} and axial symmetry to 10^{-3} using Analytic Kludge waveforms and Fisher analysis.
-
Are Black Holes Fuzzballs? Probing Horizon-Scale Structure with LISA
LISA can constrain non-axisymmetric mass quadrupole deformations at the 10^{-3} level and axisymmetric mass octupole deformations at the 10^{-2} level in EMRI signals to test fuzzball proposals.
-
Inference of recoil kicks from binary black hole mergers up to GWTC--4 and their astrophysical implications
Recoil kicks are inferred for GWTC-4 binary black hole events with values up to nearly 1000 km/s for some, yielding retention probabilities of 1-5% in globular clusters and 70-100% in elliptical galaxies.
-
Gravitational waves of extreme-mass-ratio inspirals in a rotating black hole with Dehnen dark matter halo
EMRI waveforms in a rotating black hole with Dehnen DM halo show amplitude and phase shifts from Kerr, with mismatch rising as DM mass parameter and black hole spin increase.
-
Not too close! Evaluating the impact of the baseline on the localization of binary black holes by next-generation gravitational-wave detectors
Baselines of 8-11 ms light travel time for two CE detectors provide a reasonable compromise for BBH sky localization, with third detectors eliminating multimodality for most or all events.
Reference graph
Works this paper leans on
-
[1]
K. Akiyamaet al.(Event Horizon Telescope), First Sagittar- ius A* Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole in the Center of the Milky Way, Astrophys. J. Lett.930, L12 (2022), arXiv:2311.08680 [astro- ph.HE]
work page internal anchor Pith review Pith/arXiv arXiv 2022
-
[2]
A. M. Ghezet al., Measuring Distance and Properties of the Milky Way’s Central Supermassive Black Hole with Stel- lar Orbits, Astrophys. J.689, 1044 (2008), arXiv:0808.2870 [astro-ph]
work page Pith review arXiv 2008
-
[3]
Monitoring stellar orbits around the Massive Black Hole in the Galactic Center
S. Gillessen, F. Eisenhauer, S. Trippe, T. Alexander, R. Gen- zel, F. Martins, and T. Ott, Monitoring stellar orbits around the Massive Black Hole in the Galactic Center, Astrophys. J.692, 1075 (2009), arXiv:0810.4674 [astro-ph]
work page Pith review arXiv 2009
- [4]
-
[5]
R. A. Remillard and J. E. McClintock, X-ray Properties of Black-Hole Binaries, Ann. Rev. Astron. Astrophys.44, 49 (2006), arXiv:astro-ph/0606352. 20
work page internal anchor Pith review Pith/arXiv arXiv 2006
-
[6]
B. L. Webster and P. Murdin, Cygnus X-1-a Spectroscopic Bi- nary with a Heavy Companion?, Nature235, 37 (1972)
work page 1972
-
[7]
C. T. Bolton, Identification of Cygnus X-1 with HDE 226868, Nature (London)235, 271 (1972)
work page 1972
-
[8]
Schmidt, 3C 273 : A Star-Like Object with Large Red- Shift, Nature197, 1040 (1963)
M. Schmidt, 3C 273 : A Star-Like Object with Large Red- Shift, Nature197, 1040 (1963)
work page 1963
-
[9]
P. Panuzzoet al.(Gaia), Discovery of a dormant 33 solar-mass black hole in pre-release Gaia astrometry, Astron. Astrophys. 686, L2 (2024), arXiv:2404.10486 [astro-ph.GA]
-
[10]
G. W. Gibbons, Vacuum Polarization and the Spontaneous Loss of Charge by Black Holes, Commun. Math. Phys.44, 245 (1975)
work page 1975
-
[11]
R. M. Wald, Black hole in a uniform magnetic field, Phys. Rev. D10, 1680 (1974)
work page 1974
-
[12]
M. Zajacek and A. Tursunov, The Electric Charge of Black Holes: Is It Really Always Negligible, The Observatory139, 231 (2019), arXiv:1904.04654 [astro-ph.GA]
-
[13]
P. C. Peters and J. Mathews, Gravitational radiation from point masses in a keplerian orbit, Phys. Rev.131, 435 (1963)
work page 1963
-
[14]
Post-Newtonian Theory for Gravitational Waves
L. Blanchet, Gravitational Radiation from Post-Newtonian Sources and Inspiralling Compact Binaries, Living Rev. Rel. 17, 2 (2014), arXiv:1310.1528 [gr-qc]
work page internal anchor Pith review Pith/arXiv arXiv 2014
- [15]
-
[16]
C. V . Vishveshwara, Scattering of Gravitational Radiation by a Schwarzschild Black-hole, Nature227, 936 (1970)
work page 1970
-
[17]
A. G. Doroshkevich, Y . B. Zel’dovich, and I. D. Novikov, Gravitational collapse of non-symmetric and rotating masses, Sov. Phys. JETP22, 122 (1966)
work page 1966
-
[18]
R. H. Price, Nonspherical perturbations of relativistic gravita- tional collapse. I. Scalar and gravitational perturbations, Phys. Rev. D5, 2419 (1972)
work page 1972
-
[19]
R. H. Price, Nonspherical Perturbations of Relativistic Grav- itational Collapse. II. Integer-Spin, Zero-Rest-Mass Fields, Phys. Rev. D5, 2439 (1972)
work page 1972
-
[20]
Quasinormal modes of black holes and black branes
E. Berti, V . Cardoso, and A. O. Starinets, Quasinormal modes of black holes and black branes, Class. Quant. Grav.26, 163001 (2009), arXiv:0905.2975 [gr-qc]
work page internal anchor Pith review Pith/arXiv arXiv 2009
-
[21]
S. W. Hawking, Gravitational radiation from colliding black holes, Phys. Rev. Lett.26, 1344 (1971)
work page 1971
- [22]
-
[23]
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
-
[24]
T. Akutsuet al.(KAGRA), Overview of KAGRA: Detector design and construction history, PTEP2021, 05A101 (2021), arXiv:2005.05574 [physics.ins-det]
-
[25]
S. Soniet al.(LIGO), LIGO Detector Characterization in the first half of the fourth Observing run, Class. Quant. Grav.42, 085016 (2025), arXiv:2409.02831 [astro-ph.IM]
- [26]
-
[27]
Analysis Framework for the Prompt Discovery of Compact Binary Mergers in Gravitational-wave Data
C. Messicket al., Analysis Framework for the Prompt Discov- ery of Compact Binary Mergers in Gravitational-wave Data, Phys. Rev. D95, 042001 (2017), arXiv:1604.04324 [astro- ph.IM]
work page Pith review arXiv 2017
-
[28]
S. Sachdevet al., The GstLAL Search Analysis Methods for Compact Binary Mergers in Advanced LIGO’s Sec- ond and Advanced Virgo’s First Observing Runs (2019), arXiv:1901.08580 [gr-qc]
work page Pith review arXiv 2019
-
[29]
C. Hannaet al., Fast evaluation of multidetector consistency for real-time gravitational wave searches, Phys. Rev. D101, 022003 (2020), arXiv:1901.02227 [gr-qc]
- [30]
-
[31]
L. Tsukadaet al., Improved ranking statistics of the GstLAL inspiral search for compact binary coalescences, Phys. Rev. D 108, 043004 (2023), arXiv:2305.06286 [astro-ph.IM]
-
[32]
B. Ewinget al., Performance of the low-latency GstLAL inspi- ral search towards LIGO, Virgo, and KAGRA’s fourth observ- ing run, Phys. Rev. D109, 042008 (2024), arXiv:2305.05625 [gr-qc]
-
[33]
S. Sakonet al., Template bank for compact binary merg- ers in the fourth observing run of Advanced LIGO, Ad- vanced Virgo, and KAGRA, Phys. Rev. D109, 044066 (2024), arXiv:2211.16674 [gr-qc]
-
[34]
New Methods for Offline GstLAL Analyses
P. Joshiet al., New Methods for Offline GstLAL Analyses (2025), arXiv:2506.06497 [gr-qc]
work page internal anchor Pith review Pith/arXiv arXiv 2025
-
[35]
P. Joshiet al., How Many Times Should We Matched Filter Gravitational Wave Data? A Comparison of GstLAL’s Online and Offline Performance (2025), arXiv:2505.23959 [gr-qc]
work page internal anchor Pith review Pith/arXiv arXiv 2025
- [36]
-
[37]
A. Rayet al., When to Point Your Telescopes: Gravitational Wave Trigger Classification for Real-Time Multi-Messenger Followup Observations (2023), arXiv:2306.07190 [gr-qc]
-
[38]
V . Skliris, M. R. K. Norman, and P. J. Sutton, Toward real- time detection of unmodeled gravitational wave transients us- ing convolutional neural networks, Phys. Rev. D110, 104034 (2024), arXiv:2009.14611 [astro-ph.IM]
-
[39]
Q. Chuet al., SPIIR online coherent pipeline to search for gravitational waves from compact binary coalescences, Phys. Rev. D105, 024023 (2022), arXiv:2011.06787 [gr-qc]
- [40]
-
[41]
C. All ´en´eet al., The MBTA pipeline for detecting com- pact binary coalescences in the fourth LIGO-Virgo-KAGRA observing run, Class. Quant. Grav.42, 105009 (2025), arXiv:2501.04598 [gr-qc]
-
[42]
T. Dal Canton, A. H. Nitz, B. Gadre, G. S. Cabourn Davies, V . Villa-Ortega, T. Dent, I. Harry, and L. Xiao, Real-time Search for Compact Binary Mergers in Advanced LIGO and Virgo’s Third Observing Run Using PyCBC Live, Astrophys. J.923, 254 (2021), arXiv:2008.07494 [astro-ph.HE]
-
[43]
S. Klimenkoet al., Method for detection and reconstruction of gravitational wave transients with networks of advanced de- tectors, Phys. Rev. D93, 042004 (2016), arXiv:1511.05999 [gr-qc]
work page Pith review arXiv 2016
- [44]
-
[45]
B. S. Sathyaprakash and S. V . Dhurandhar, Choice of filters for the detection of gravitational waves from coalescing binaries, Phys. Rev. D44, 3819 (1991)
work page 1991
- [46]
-
[47]
A. G. Abacet al.(LIGO Scientific, Virgo, KAGRA), GW230814: investigation of a loud gravitational-wave signal observed with a single detector, LIGO-P230814 (2025)
work page 2025
- [48]
-
[49]
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 arXiv 2021
-
[50]
M. Colleoni, F. A. R. Vidal, C. Garc ´ıa-Quir´os, S. Akc ¸ay, 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]
-
[51]
L. Pompiliet al., Laying the foundation of the effective- one-body waveform models SEOBNRv5: Improved accuracy and efficiency for spinning nonprecessing binary black holes, Phys. Rev. D108, 124035 (2023), arXiv:2303.18039 [gr-qc]
-
[52]
M. Khalil, A. Buonanno, H. Estelles, D. P. Mihaylov, S. Ossokine, L. Pompili, and A. Ramos-Buades, Theoretical groundwork supporting the precessing-spin two-body dynam- ics of the effective-one-body waveform models SEOBNRv5, Phys. Rev. D108, 124036 (2023), arXiv:2303.18143 [gr-qc]
-
[53]
M. van de Meent, A. Buonanno, D. P. Mihaylov, S. Ossokine, L. Pompili, N. Warburton, A. Pound, B. Wardell, L. Durkan, and J. Miller, Enhancing the SEOBNRv5 effective-one-body waveform model with second-order gravitational self-force fluxes, Phys. Rev. D108, 124038 (2023), arXiv:2303.18026 [gr-qc]
-
[54]
A. Ramos-Buades, A. Buonanno, H. Estell ´es, M. Khalil, D. P. Mihaylov, S. Ossokine, L. Pompili, and M. Shiferaw, Next generation of accurate and efficient multipolar precessing-spin effective-one-body waveforms for binary black holes, Phys. Rev. D108, 124037 (2023), arXiv:2303.18046 [gr-qc]
-
[55]
E. Hamilton, L. London, J. E. Thompson, E. Fauchon-Jones, M. Hannam, C. Kalaghatgi, S. Khan, F. Pannarale, and A. Vano-Vinuales, Model of gravitational waves from precess- ing black-hole binaries through merger and ringdown, Phys. Rev. D104, 124027 (2021), arXiv:2107.08876 [gr-qc]
-
[56]
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 bi- naries with higher multipoles and asymmetries, Phys. Rev. D 109, 063012 (2024), arXiv:2312.10025 [gr-qc]
-
[57]
A. Gamboaet al., Accurate waveforms for eccentric, aligned- spin binary black holes: The multipolar effective-one- body model SEOBNRv5EHM, Phys. Rev. D , (2025), arXiv:2412.12823 [gr-qc]
- [58]
-
[59]
A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), GWTC-4.0: Population Properties of Merging Compact Bi- naries (2025), arXiv:2508.18083 [astro-ph.HE]
work page internal anchor Pith review Pith/arXiv arXiv 2025
- [60]
- [61]
- [62]
-
[63]
Algebraic Classification of Numerical Spacetimes and Black-Hole-Binary Remnants
M. Campanelli, C. O. Lousto, and Y . Zlochower, Alge- braic Classification of Numerical Spacetimes and Black- Hole-Binary Remnants, Phys. Rev. D79, 084012 (2009), arXiv:0811.3006 [gr-qc]
work page Pith review arXiv 2009
-
[64]
W. H. Press, Long Wave Trains of Gravitational Waves from a Vibrating Black Hole, Astrophys. J. Lett.170, L105 (1971)
work page 1971
- [65]
-
[66]
S. A. Teukolsky, Perturbations of a rotating black hole. 1. Fun- damental equations for gravitational electromagnetic and neu- trino field perturbations, Astrophys. J.185, 635 (1973)
work page 1973
-
[67]
S. Chandrasekhar and S. L. Detweiler, The quasi-normal modes of the Schwarzschild black hole, Proc. Roy. Soc. Lond. A344, 441 (1975)
work page 1975
- [68]
-
[69]
A. Hussain and A. Zimmerman, Approach to computing spec- tral shifts for black holes beyond Kerr, Phys. Rev. D106, 104018 (2022), arXiv:2206.10653 [gr-qc]
- [70]
- [71]
-
[72]
V . Cardoso, M. Kimura, A. Maselli, and L. Senatore, Black Holes in an Effective Field Theory Extension of General Relativity, Phys. Rev. Lett.121, 251105 (2018), [Erratum: Phys.Rev.Lett. 131, 109903 (2023)], arXiv:1808.08962 [gr- qc]
- [73]
- [74]
- [75]
-
[76]
L. Pierini and L. Gualtieri, Quasi-normal modes of rotating black holes in Einstein-dilaton Gauss-Bonnet gravity: the first order in rotation, Phys. Rev. D103, 124017 (2021), arXiv:2103.09870 [gr-qc]
-
[77]
L. Pierini and L. Gualtieri, Quasinormal modes of rotating black holes in Einstein-dilaton Gauss-Bonnet gravity: The second order in rotation, Phys. Rev. D106, 104009 (2022), arXiv:2207.11267 [gr-qc]
- [78]
- [79]
- [80]
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.