The first informative astrophysical calibration of gravitational-wave detectors is reported using GW240925 and GW250207.
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GWTC-4.0: Updating the Gravitational-Wave Transient Catalog with Observations from the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run
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abstract
Version 4.0 of the Gravitational-Wave Transient Catalog (GWTC-4.0) adds new candidates detected by the LIGO, Virgo, and KAGRA observatories through the first part of the fourth observing run (O4a: 2023 May 24 15:00:00 to 2024 January 16 16:00:00 UTC) and a preceding engineering run. In this new data, we find 128 new compact binary coalescence candidates that are identified by at least one of our search algorithms with a probability of astrophysical origin $p_{\rm astro} \geq 0.5$ and that are not vetoed during event validation. We also provide detailed source property measurements for 86 of these that have a false alarm rate $< 1 \rm{yr}^{-1}$. Based on the inferred component masses, these new candidates are consistent with signals from binary black holes and neutron star-black hole binaries (GW230518_125908 and GW230529_181500). Median inferred component masses of binary black holes in the catalog now range from $5.79\,M_\odot$ (GW230627_015337) to $137\,M_\odot$ (GW231123_135430), while GW231123_135430 was probably produced by the most massive binary observed in the catalog. For the first time we have discovered binary black hole signals with network signal-to-noise ratio exceeding 30, GW230814_230901 and GW231226_01520, enabling high-fidelity studies of the waveforms and astrophysical properties of these systems. Combined with the 90 candidates included in GWTC-3.0, the catalog now contains 218 candidates with $p_{\rm astro} \geq 0.5$ and not otherwise vetoed, doubling the size of the catalog and further opening our view of the gravitational-wave Universe.
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- abstract Version 4.0 of the Gravitational-Wave Transient Catalog (GWTC-4.0) adds new candidates detected by the LIGO, Virgo, and KAGRA observatories through the first part of the fourth observing run (O4a: 2023 May 24 15:00:00 to 2024 January 16 16:00:00 UTC) and a preceding engineering run. In this new data, we find 128 new compact binary coalescence candidates that are identified by at least one of our search algorithms with a probability of astrophysical origin $p_{\rm astro} \geq 0.5$ and that are not vetoed during event validation. We also provide detailed source property measurements for 86 of th
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representative citing papers
The first search for scalar-induced gravitational waves via pulsar parameter drifts yields f_PBH < 10^{-10} (95% CL) for PBH masses 0.3 to 4e4 solar masses, strongly disfavoring a primordial black hole origin for LVK binary black holes.
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.
Gravitational memory from hairy binary black hole mergers in scalar-Gauss-Bonnet gravity differs from GR by a few percent due to altered nonlinear dynamics, with direct scalar contributions suppressed, and including memory increases GR-sGB mismatch by more than an order of magnitude.
First joint population inference on binary black hole eccentricity from GWTC-4 bounds the eccentric branching ratio below 5% at 90% confidence, with results consistent with quasi-circular models but highly model-dependent.
Coincident anomaly detection trains neural networks on detector coincidence to find gravitational-wave events without templates, reaching recall 0.91 at one false alarm per year on injected signals.
Presents new NSBH waveform models IMRPhenomXHM_NSBH, SEOBNRv5HM_ROM_NRTidalv3_NSBH, and IMRPhenomXPHM_NSBH incorporating higher modes and tidal effects via NRTidalv3 extensions, validated against NR simulations and applied to GWTC events.
Introduces regression on regression to fit physical parameters (τ_min, α, A, γ, δ) to GWTC-4 B-Spline merger rate posteriors, finding the progenitor formation rate evolves ~5.3 times steeper than the star formation rate at low z and exposing model misspecification.
SEOBNRv6EHM is a multipolar EOB model for eccentric planar-orbit BBHs calibrated to NR simulations, showing low waveform mismatches up to eccentricity 0.9.
A contrastive self-supervised convolutional autoencoder detects core-collapse supernova gravitational waves with performance comparable to supervised CNNs, better generalization to unseen waveforms, and ~120 kpc sensitive distance under Einstein Telescope noise.
A reference-frequency-independent detection statistic for eccentric binary mergers is introduced and applied to GW200105, yielding ln B ≤ 0.9 in favor of the eccentric aligned-spin model over the quasi-circular precessing model.
Natural polynomials for Schwarzschild and Kerr quasinormal modes are Pollaczek-Jacobi polynomials with complex parameters, with recurrence peaking at the physical overtone index for Schwarzschild.
Dingo-Pop uses a transformer to perform amortized, end-to-end population inference from GW strain data in seconds, bypassing per-event Monte Carlo sampling.
A traceful radiation gauge plus two transport equations from the stress-energy tensor enable hierarchical metric reconstruction for generic sources in Petrov type D black hole spacetimes.
GW-Eyes is a new LLM-powered agent framework that autonomously associates gravitational-wave events with electromagnetic counterparts by integrating specialized tools and supporting natural-language interaction.
Multiband observations of eccentric binary black holes can constrain dipole-radiation deviations from general relativity to |b| ≲ 10^{-7} for a GW231123-like event when combining one year of space-based data with ground-informed priors.
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 signals degenerate until IMR consistency tests are applied.
Derives large-eccentricity asymptotics for post-Newtonian eccentric waveform Fourier modes and builds a fast endpoint-constrained analytic approximation with error under 10^{-3} valid to p=200.
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.
The gwNRHME framework constructs a multi-modal non-spinning eccentric gravitational waveform surrogate by modulating quasi-circular models with universal eccentric functions, achieving median mismatches of ~9e-5 against 156 NR 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 dynamical parameters.
Labrador is a domain-optimized neural posterior estimation tool achieving 1% median importance-sampling efficiency and first extensive coverage of long-duration low-mass gravitational wave signals through equivariance and a stable procedure for differing priors.
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.
Joint analysis of LVK standard sirens and DES 3x2pt data yields H0 = 67.9 +4.4/-4.3 km s^{-1} Mpc^{-1} at 6.4% precision while tightening the Omega_m constraint by 22%.
citing papers explorer
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GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors
The first informative astrophysical calibration of gravitational-wave detectors is reported using GW240925 and GW250207.
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Constraints on the Primordial Black Hole Abundance using Pulsar Parameter Drifts
The first search for scalar-induced gravitational waves via pulsar parameter drifts yields f_PBH < 10^{-10} (95% CL) for PBH masses 0.3 to 4e4 solar masses, strongly disfavoring a primordial black hole origin for LVK binary black holes.
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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.
-
Gravitational Memory from Hairy Binary Black Hole Mergers
Gravitational memory from hairy binary black hole mergers in scalar-Gauss-Bonnet gravity differs from GR by a few percent due to altered nonlinear dynamics, with direct scalar contributions suppressed, and including memory increases GR-sGB mismatch by more than an order of magnitude.
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Population Properties of Binary Black Holes with Eccentricity
First joint population inference on binary black hole eccentricity from GWTC-4 bounds the eccentric branching ratio below 5% at 90% confidence, with results consistent with quasi-circular models but highly model-dependent.
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Template-free search for gravitational wave events using coincident anomaly detection
Coincident anomaly detection trains neural networks on detector coincidence to find gravitational-wave events without templates, reaching recall 0.91 at one false alarm per year on injected signals.
-
Fast gravitational waveform models for quasi-circular coalescences of neutron star--black hole binaries
Presents new NSBH waveform models IMRPhenomXHM_NSBH, SEOBNRv5HM_ROM_NRTidalv3_NSBH, and IMRPhenomXPHM_NSBH incorporating higher modes and tidal effects via NRTidalv3 extensions, validated against NR simulations and applied to GWTC events.
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Regression on Regression: Mapping Data-Driven Binary Black Hole Merger Rate Fits to Progenitor Histories
Introduces regression on regression to fit physical parameters (τ_min, α, A, γ, δ) to GWTC-4 B-Spline merger rate posteriors, finding the progenitor formation rate evolves ~5.3 times steeper than the star formation rate at low z and exposing model misspecification.
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Accurate waveforms for generic planar-orbit binary black holes: The multipolar effective-one-body model SEOBNRv6EHM
SEOBNRv6EHM is a multipolar EOB model for eccentric planar-orbit BBHs calibrated to NR simulations, showing low waveform mismatches up to eccentricity 0.9.
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Contrastive self-supervised convolutional autoencoder for core-collapse supernova gravitational-wave detection
A contrastive self-supervised convolutional autoencoder detects core-collapse supernova gravitational waves with performance comparable to supervised CNNs, better generalization to unseen waveforms, and ~120 kpc sensitive distance under Einstein Telescope noise.
-
A universal framework to identify eccentric binary mergers: GW200105 case study
A reference-frequency-independent detection statistic for eccentric binary mergers is introduced and applied to GW200105, yielding ln B ≤ 0.9 in favor of the eccentric aligned-spin model over the quasi-circular precessing model.
-
Properties of natural polynomials for Schwarzschild and Kerr black holes
Natural polynomials for Schwarzschild and Kerr quasinormal modes are Pollaczek-Jacobi polynomials with complex parameters, with recurrence peaking at the physical overtone index for Schwarzschild.
-
End-to-End Population Inference from Gravitational-Wave Strain using Transformers
Dingo-Pop uses a transformer to perform amortized, end-to-end population inference from GW strain data in seconds, bypassing per-event Monte Carlo sampling.
-
Metric Reconstruction for Generic Black-Hole Perturbations
A traceful radiation gauge plus two transport equations from the stress-energy tensor enable hierarchical metric reconstruction for generic sources in Petrov type D black hole spacetimes.
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An agentic framework for gravitational-wave counterpart association in the multi-messenger era
GW-Eyes is a new LLM-powered agent framework that autonomously associates gravitational-wave events with electromagnetic counterparts by integrating specialized tools and supporting natural-language interaction.
-
Constraining Dipole Radiation with Multiband Gravitational Waves from Eccentric Binary Black Holes
Multiband observations of eccentric binary black holes can constrain dipole-radiation deviations from general relativity to |b| ≲ 10^{-7} for a GW231123-like event when combining one year of space-based data with ground-informed priors.
-
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 signals degenerate until IMR consistency tests are applied.
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Large-Eccentricity Asymptotics and Fast Analytic Approximation for Fourier modes of Post-Newtonian Eccentric Waveforms
Derives large-eccentricity asymptotics for post-Newtonian eccentric waveform Fourier modes and builds a fast endpoint-constrained analytic approximation with error under 10^{-3} valid to p=200.
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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.
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Including higher-order modes in a quadrupolar eccentric numerical relativity surrogate using universal eccentric modulation functions
The gwNRHME framework constructs a multi-modal non-spinning eccentric gravitational waveform surrogate by modulating quasi-circular models with universal eccentric functions, achieving median mismatches of ~9e-5 against 156 NR waveforms.
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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 dynamical parameters.
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labrador: A domain-optimized machine-learning tool for gravitational wave inference
Labrador is a domain-optimized neural posterior estimation tool achieving 1% median importance-sampling efficiency and first extensive coverage of long-duration low-mass gravitational wave signals through equivariance and a stable procedure for differing priors.
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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.
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First measurement of the Hubble constant from a combined weak lensing and gravitational-wave standard siren analysis
Joint analysis of LVK standard sirens and DES 3x2pt data yields H0 = 67.9 +4.4/-4.3 km s^{-1} Mpc^{-1} at 6.4% precision while tightening the Omega_m constraint by 22%.
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Search for Precessing Binary Black Holes in Advanced LIGO's Third Observing Run using Harmonic Decomposition
A new harmonic-decomposition template search for precessing binary black holes in LIGO O3 data improves sensitivity by up to 28% and reduces computational cost by up to 5x with no new detections.
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Mind the peak: improving cosmological constraints from GWTC-4.0 spectral sirens using semiparametric mass models
A data-driven Bspline model for the binary black hole mass distribution from 137 GW events resolves three peaks and improves H0 precision by 12-21% over parametric alternatives.
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The First Model-Independent Upper Bound on Micro-lensing Signature of the Highest Mass Binary Black Hole Event GW231123
No definitive lensing is detected in GW231123, though a potential microlensing feature with modulation amplitude up to 0.8 at 95% confidence is noted, limited by large waveform systematics in short signals.
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Observational constraints on the spin/anisotropy of the CCOs of Cassiopeia A, Vela Jr. and G347.3-0.5 and a single surviving continuous gravitational wave candidate
New upper limits on gravitational-wave amplitude, ellipticity below 4e-7 for fast spins, and crustal anisotropy below 5e-3 for 1.3-100 ms periods from Cas A, Vela Jr., and G347.3-0.5, plus one surviving candidate.
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Black hole mergers beyond general relativity: a self-force approach
Self-force theory is extended to compute merger and ringdown waveforms in beyond-GR black hole binaries under the extreme mass-ratio approximation, with first calculations of self-force corrections to the merger waveform.
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Artificial Precision Timing Array: bridging the decihertz gravitational-wave sensitivity gap with clock satellites
Proposes APTA with 6 satellites and 10^{-18} relative clock uncertainty at 1s averaging to achieve sensitivity for observing 10^3-10^4 solar-mass black hole mergers in the decihertz band.
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A Strongly Parametrized Mass Ratio Model for the Stable Mass Transfer Channel: a Case Study of the $10 \, \rm{M}_{\odot}$ Peak
A parametrized analytical model for BBH mass ratios from the stable mass transfer channel is derived and applied to the 10 solar-mass peak in GWTC-4, favoring little mass-ratio reversal.
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Rapidly Rotating Neutron Star Collapse in Massive Scalar-Tensor Theories
Numerical simulations of collapsing scalarized neutron stars show scalar radiation energy of order 10^{-3} solar masses, orders of magnitude above the tensor quadrupolar emission, potentially observable to test modified gravity.
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Detectability of avoided crossings in black hole ringdowns
Bayesian analysis finds individual QNM frequencies near avoided crossings hard to resolve even under optimistic conditions, though collective AC waveform signatures may remain detectable if those modes dominate and slower-mode contamination is minimal.
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Polarization Analysis of Ringdown Signals
Constrained polarization model for Kerr ringdown modes enables inclination inference from two-detector data for non-precessing mergers but introduces biases when applied to precessing systems.
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N-body next-to-leading order gravitational spin-orbit interaction via effective field theory
The NLO gravitational spin-orbit Hamiltonian for N spinning bodies is computed via PN-EFT, with only three-body diagrams new beyond the binary case, and the result matches the known ADM Hamiltonian up to canonical transformation.
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Prospects for multi-messenger discovery of the gravitational-wave background anisotropies via cross-correlation with galaxies
New simulations show that cross-correlating gravitational wave background anisotropies with galaxy distributions can enable discovery at angular scales of 4-6 degrees with next-generation observatories.
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Implications of the LISA stochastic signal from eccentric stellar mass black hole binaries in vacuum
High initial eccentricities in stellar-mass black hole binaries produce a stochastic gravitational wave background distinguishable by LISA from quasi-circular models, enabling upper bounds on eccentricity and separation of environmental effects for dense gas.
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Merger remnant and eccentricity dynamics surrogates for eccentric nonspinning black hole binaries
Two new surrogate models, trained on NR simulations, predict remnant properties and eccentricity dynamics for nonspinning eccentric black hole binaries with q ≤ 4 and e < 0.23.
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Normalizing flows for density estimation in multi-detector gravitational-wave searches
Normalizing flows replace binned histograms for estimating multi-detector signal parameters in PyCBC, slashing storage by three orders of magnitude with under 0.05% sensitivity loss and up to 6.55% gains in specific cases.
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Interpretable Analytic Formulae for GWTC-4 Binary Black Hole Population Properties via Symbolic Regression
Symbolic regression on GWTC-4 posteriors yields closed-form analytic formulae for merger-rate evolution, effective-spin dependencies on mass ratio and redshift, and conditional mass-ratio distributions at specific primary mass peaks.
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Parameter Estimation of the Gravitational-Wave Angular Power Spectrum in the Dirty-Map Space
A dirty-map space inference method allows recovery of SGWB angular power spectrum parameters from LIGO O3 simulations for strong signals in auto- and cross-correlation searches up to ℓ_max=10.
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Boson star-black hole binaries: initial data and head-on collisions
A one-body conformal-factor correction stabilizes boson star-black hole initial data, enabling gravitational-wave analysis that shows higher multipoles can discriminate mixed mergers from pure black-hole binaries.
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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.
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Post-Newtonian inspiral waveform model for eccentric precessing binaries with higher-order modes and matter effects
pyEFPEHM extends prior PN models to include higher-order quasi-circular phasing, generalized precession solutions, and eccentric corrections up to 1PN in selected multipoles for eccentric precessing binaries with matter effects.
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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}.
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Repopulating the pair-instability mass gap without sustained growth to massive IMBHs: the case of 47\,Tuc
Simulations of 47 Tuc show hierarchical mergers and occasional surviving primordial seeds above the pair-instability gap produce retained black holes of 45-1100 solar masses with distinct spin distributions, favoring a dark-remnant population over a single massive IMBH while remaining consistent the
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Posterior Predictive Checks for Gravitational-wave Populations: Limitations and Improvements
Maximum-likelihood-based posterior predictive checks detect model misspecification better than event-level versions for uncertain spin tilts, but current detector sensitivity limits their power; the Gaussian Component Spins model underpredicts high spin magnitudes and overpredicts anti-aligned tilts
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Self-gravitating thin shells are dynamically unstable on all angular scales
Self-gravitating thin shells in general relativity are dynamically unstable on all angular scales, exhibiting an exponentially growing mode for all sampled compactness, adiabatic index, and multipole order ℓ ≥ 2.
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Particle motions and gravitational waveforms in rotating black hole spacetimes of loop quantum gravity
The LQG parameter ξ enlarges equatorial bound orbit energy ranges, confines off-equatorial trajectories, and produces larger deviations from Kerr waveforms in EMRI models for two rotating LQG black holes, though signals fall below detector sensitivities.
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Kerr Black Hole Ringdown in Effective Field Theory
Effective field theory yields model-independent corrections to Kerr black hole quasinormal modes that oscillate logarithmically near extremality, indicating discrete scale invariance.