A cross-correlation search of ~11,000 event pairs in GWTC-4 including sub-threshold candidates finds no lensed GW pairs above 3σ, setting an upper bound of ≤1.5/yr on the lensing rate.
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GWTC-4.0: Constraints on the Cosmic Expansion Rate and Modified Gravitational-wave Propagation
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abstract
We analyze data from 142 of the 218 gravitational-wave (GW) sources in the fourth LIGO-Virgo-KAGRA Collaboration (LVK) Gravitational-Wave Transient Catalog (GWTC-4.0) to estimate the Hubble constant $H_0$ jointly with the population properties of merging compact binaries. We measure the luminosity distance and redshifted masses of GW sources directly; in contrast, we infer GW source redshifts statistically through i) location of features in the compact object mass spectrum and merger rate evolution, and ii) identifying potential host galaxies in the GW localization volume. Probing the relationship between source luminosity distances and redshifts obtained in this way yields constraints on cosmological parameters. We also constrain parameterized deviations from general relativity which affect GW propagation, specifically those modifying the dependence of a GW signal on the source luminosity distance. Assuming our fiducial model for the source-frame mass distribution and using GW candidates detected up to the end of the fourth observing run (O4a), together with the GLADE+ all-sky galaxy catalog, we estimate $H_0 = 76.6^{+13.0}_{-9.5} (76.6^{+25.2}_{-14.0})$ km s$^{-1}$ Mpc$^{-1}$. This value is reported as a median with 68.3% (90%) symmetric credible interval, and includes combination with the $H_0$ measurement from GW170817 and its electromagnetic counterpart. Using a parametrization of modified GW propagation in terms of the magnitude parameter $\Xi_0$, we estimate $\Xi_0 = 1.2^{+0.8}_{-0.4} (1.2^{+2.4}_{-0.5})$, where $\Xi_0 = 1$ recovers the behavior of general relativity.
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2026 30representative citing papers
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.
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.
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.
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%.
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.
Simulations for Einstein Telescope and Cosmic Explorer forecast that decade-scale samples of strongly lensed GWs can constrain the cosmic dipole magnitude at the few×10^{-3} level when combined with multi-image events.
O4a gravitational-wave data give 95% CL upper limits f_PBH ~ 1e-2 to 1e-4 for monochromatic primordial black holes with mean masses 0.6-100 M_sun, with no evidence of a PBH merger component.
Using simulated binary black hole mergers and neutral hydrogen maps, the radio sirens method constrains H0 to 8% precision with 3000 high-SNR events, offering a 90% improvement over standard dark siren analyses.
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.
A glitch-robust amortized inference framework combining normalizing flows, time-frequency multimodal fusion, and contrastive learning outperforms MCMC for Taiji massive black hole binary parameter estimation under noise contamination.
The GW-galaxy cross-correlation method, unified with spectral sirens in a harmonic framework, can measure H0 to 1% and Omega_m to 5% precision with 2 years of data from next-generation detectors like Einstein Telescope and Cosmic Explorer.
Simulations show a 40-50 solar-mass black-hole cutoff is not guaranteed to be confidently recovered from GWTC-4-like catalogs, spurious detections are unlikely, and O4 data would reduce cutoff-mass uncertainty by at least 20 percent while yielding only a lower bound on the carbon-alpha reaction rate
Third-generation gravitational-wave detectors can constrain frequency-dependent beyond-GR waveform modifications in the stochastic background, but modified propagation effects remain degenerate with astrophysical population parameters.
ET-Δ outperforms ET-2L on luminosity distance and source-frame masses for BBH events because its redundancy produces higher multi-detector uptime under realistic duty-cycle modeling.
Combining GWTC-4 standard sirens with TDCOSMO2025 lensing data under the distance sum rule yields H0 = 83.78 +12.53/-10.23 km/s/Mpc (13.6% precision) in one configuration, consistent with both Planck and SH0ES.
Spectral-siren H0 constraints from GWTC-4.0 binary black holes remain robust when the mass spectrum is permitted to evolve with redshift at current detector sensitivity.
Waveform modeling uncertainties can distort features in the binary black hole mass distribution inferred from gravitational-wave data more than statistical uncertainties.
Derives multimessenger consistency relations for luminosity distances in the Friedmann model, including a curvature parameter expressed solely in terms of flatness-biased distances and a cosmological-constant relation independent of flatness assumptions.
B-spline agnostic reconstruction of binary black hole masses from GWTC-4.0 reveals multiple features and a logarithmic hierarchy that impacts Hubble constant measurements, with a low-mass subpopulation isolation method to mitigate systematics.
Next-generation GW detector networks can constrain the spatial curvature parameter Ω_k to 1σ uncertainty of 0.029 using intermediate-mass binary black hole bright sirens.
GPU-accelerated gwcosmo enables 1000x faster dark-siren cosmological analyses for large GW catalogs.
Reanalysis of flagged LVK events with waveform uncertainty models produces consistent spin and precession inferences across raw/deglitched data and multiple waveform approximants.
VIGILant applies tree-based models and a ResNet CNN to classify Virgo O3b glitches with 98% accuracy and has been deployed for daily use with an interactive dashboard.
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Model-Independent Search Discards Faint Lensed-Pairs of Gravitational Wave Events in the Sub-Threshold Candidates of GWTC-4
A cross-correlation search of ~11,000 event pairs in GWTC-4 including sub-threshold candidates finds no lensed GW pairs above 3σ, setting an upper bound of ≤1.5/yr on the lensing rate.
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End-to-End Population Inference from Gravitational-Wave Strain using Transformers
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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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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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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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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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Prospect of Measuring the Cosmic Dipole by Associating Strongly Lensed Gravitational Waves with Galaxy Surveys
Simulations for Einstein Telescope and Cosmic Explorer forecast that decade-scale samples of strongly lensed GWs can constrain the cosmic dipole magnitude at the few×10^{-3} level when combined with multi-image events.
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Constraints on primordial black holes from the first part of LIGO-Virgo-KAGRA fourth observing run
O4a gravitational-wave data give 95% CL upper limits f_PBH ~ 1e-2 to 1e-4 for monochromatic primordial black holes with mean masses 0.6-100 M_sun, with no evidence of a PBH merger component.
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Radio sirens: inferring $H_0$ with binary black holes and neutral hydrogen in the era of the Einstein Telescope and the SKA Observatory
Using simulated binary black hole mergers and neutral hydrogen maps, the radio sirens method constrains H0 to 8% precision with 3000 high-SNR events, offering a 90% improvement over standard dark siren analyses.
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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.
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Robust parameter inference for Taiji via time-frequency contrastive learning and normalizing flows
A glitch-robust amortized inference framework combining normalizing flows, time-frequency multimodal fusion, and contrastive learning outperforms MCMC for Taiji massive black hole binary parameter estimation under noise contamination.
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A unified harmonic framework for dark siren cosmology
The GW-galaxy cross-correlation method, unified with spectral sirens in a harmonic framework, can measure H0 to 1% and Omega_m to 5% precision with 2 years of data from next-generation detectors like Einstein Telescope and Cosmic Explorer.
-
Measurement prospects for the pair-instability mass cutoff with gravitational waves
Simulations show a 40-50 solar-mass black-hole cutoff is not guaranteed to be confidently recovered from GWTC-4-like catalogs, spurious detections are unlikely, and O4 data would reduce cutoff-mass uncertainty by at least 20 percent while yielding only a lower bound on the carbon-alpha reaction rate
-
Modeling Uncertainties in Modified Gravity Predictions for the Stochastic Gravitational-Wave Background
Third-generation gravitational-wave detectors can constrain frequency-dependent beyond-GR waveform modifications in the stochastic background, but modified propagation effects remain degenerate with astrophysical population parameters.
-
Impact of the Einstein Telescope's duty cycle on the estimation of binary black holes parameters
ET-Δ outperforms ET-2L on luminosity distance and source-frame masses for BBH events because its redundancy produces higher multi-detector uptime under realistic duty-cycle modeling.
-
Model-independent H0 from GWTC-4 standard sirens and TDCOSMO 2025 strong lensing time delays
Combining GWTC-4 standard sirens with TDCOSMO2025 lensing data under the distance sum rule yields H0 = 83.78 +12.53/-10.23 km/s/Mpc (13.6% precision) in one configuration, consistent with both Planck and SH0ES.
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Gravitational-wave constraints on $H_0$ are robust to (putative) redshift evolution in the binary black hole mass spectrum at current sensitivity
Spectral-siren H0 constraints from GWTC-4.0 binary black holes remain robust when the mass spectrum is permitted to evolve with redshift at current detector sensitivity.
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Is the Binary Black Hole Population Inference from Gravitational-Wave Data Robust?
Waveform modeling uncertainties can distort features in the binary black hole mass distribution inferred from gravitational-wave data more than statistical uncertainties.
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Testing the consistency of cosmological models with multimessenger astronomy
Derives multimessenger consistency relations for luminosity distances in the Friedmann model, including a curvature parameter expressed solely in terms of flatness-biased distances and a cosmological-constant relation independent of flatness assumptions.
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Emergent structure in the binary black hole mass distribution and implications for population-based cosmology
B-spline agnostic reconstruction of binary black hole masses from GWTC-4.0 reveals multiple features and a logarithmic hierarchy that impacts Hubble constant measurements, with a low-mass subpopulation isolation method to mitigate systematics.
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Shape of U: Measuring the Curvature of the Universe with Gravitational Waves
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Scalable Dark Siren Cosmology with gwcosmo: GPU Acceleration, Validation and Systematics
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Mitigating Systematic Errors in Parameter Estimation of Binary Black Hole Mergers in O1-O3 LIGO-Virgo Data
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VIGILant: an automatic classification pipeline for glitches in the Virgo detector
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Investigating the effect of sensitivity of KAGRA on sky localization of gravitational-wave sources from compact binary coalescences
KAGRA enhances sky localization of binary neutron star mergers in the LVK network via added baselines, with measurable gains at current sensitivity and larger improvements as range reaches ~30 Mpc.
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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.
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Gravitational-wave standard sirens and application in cosmology
Review of gravitational-wave standard sirens from binary mergers for cosmology, covering distance/redshift methods, detector capabilities, and prospects for bright, dark, and lensed sirens.
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Love numbers of black holes and compact objects
A pedagogical review of Love numbers and tidal responses for black holes and compact objects in general relativity and extensions.
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The first decade of gravitational-wave measurements of black hole spins
A decade of gravitational-wave data shows most merging stellar-mass black holes have small spins, with subdominant fast-spinning, misaligned, and hierarchical-merger populations.
- GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors