Aframe neural network achieves matched-filter sensitivity for binary neutron star GW searches at lower computational cost using heterodyning and a single GPU.
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GWTC-5.0: Population Properties of Merging Compact Binaries
22 Pith papers cite this work, alongside 2 external citations. Polarity classification is still indexing.
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abstract
We present the population properties of merging compact binaries inferred using 267 mergers from the cumulative Gravitational-Wave Transient Catalog 5.0. As this data set contains no new sources with a neutron star, we primarily focus on the properties of the binary black hole mergers. We infer the merger rate of binary black holes with component masses between $2.5\,\mathrm{M}_\odot $ and $200\,\mathrm{M}_\odot $ to be $27.5\text{--} 49.4 \, \mathrm{Gpc}^{-3}\,\mathrm{yr}^{-1}$ (all intervals at $90\%$ credible levels) at redshift $z = 0.2$. We find evidence for a subpopulation of binary black hole mergers that host a rapidly spinning black hole (dimensionless spins $\chi \sim 0.7$), consistent with signatures of hierarchical mergers. We find that these occur at two mass scales, the first at primary masses $\sim 10$--$20\,\mathrm{M}_\odot $ and the second above $\sim 45\,\mathrm{M}_\odot $, and we estimate their total rate at $z=0.2$ to be $0.2\text{--} 3.11 \, {\rm Gpc}^{-3} {\rm yr}^{-1}$. We infer that, above $40\,\mathrm{M}_\odot $, the mass distribution of the less massive (secondary) black hole declines more steeply than that of the more massive (primary) one. This is consistent with a flatter mass-ratio distribution and indicates the prevalence of unequal-mass binaries with large primary masses. We find evidence for two features in the black hole mass spectrum: a peak around $10\,\mathrm{M}_\odot $ and a change of slope at around $35\,\mathrm{M}_\odot $. Black holes of $\sim 35\,\mathrm{M}_\odot $ pair preferentially with companions of similar mass. Additionally, we find that the effective inspiral spin distribution of binary black holes is asymmetric about zero, based on which we infer that at least $9 \%$ of mergers occur in channels with some preference for spin-orbit alignment. We find evidence that...
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2026 22representative citing papers
Milky Way globular clusters formed with initial half-mass densities of ~10^6.4 M_sun/pc^3, bottom-light IMFs, and small present-day black hole mass fractions, inferred by coupling rapid evolution models with multimass equilibrium models fitted to present-day observations.
All five NSBH events are consistent with zero line-of-sight acceleration; the joint posterior for GW200105_162426 disfavors both zero LOSA and zero eccentricity at 90% credibility.
Authors synthesize SVD-based reduced-order models from wave-optics simulations to provide an effective stochastic description of stellar microlensing distortions on lensed gravitational waves.
Hierarchical Bayesian analysis of GWTC-5.0 data identifies a mass transition at 15.2 solar masses separating distinct effective-spin distributions, pointing to different formation channels for low-mass binary black holes.
No GWTC-3 event robustly prefers a non-BBH merger morphology once low-frequency cutoffs are raised; apparent low-compactness modes are noise artifacts, with GW231123 left as an unresolved special case.
Joint strong-lensing and population inference on resolved gravitational-wave events finds no lensed events and tightens constraints on the black-hole merger rate peak redshift and high-redshift tail.
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Models BBH spin-orbit alignment as random walk on sphere, deriving exact distribution after n encounters and showing alignment survives several strong encounters before isotropy.
GWTC-5 chirp-mass peaks form a ~1.9-spaced ladder with a new ~19 M⊙ rung matching predicted 2G+3G mergers, unifying prior 1G+2G spin-transition groups under one hierarchical scenario.
Hierarchical Bayesian analysis of GWTC-5 binary black hole spins finds no evidence for superradiant axions and excludes masses 1.7e-14 to 3.3e-12 eV at 95% CL.
GWTC-5 population analysis finds high-spin black hole mass function traces low-spin remnant distribution with Bhattacharyya coefficient ~0.95, supporting hierarchical mergers and yielding a nuclear S-factor constraint.
Bilby-antiglitch jointly models astrophysical signals and quasi-physical glitches to recover true source properties from simulated gravitational wave data contaminated by loud non-Gaussian transients.
Stable mass transfer produces two distinct peaks in merging binary black hole primary mass and mass ratio distributions via mass ratio reversal under conservative mass transfer.
A non-parametric reconstruction of the GWTC-5 black-hole population finds a separate high-mass subpopulation (M1 ≳ 50 M☉) with positively aligned spins (χ_eff ≈ 0.4).
An idealized Gaussian model demonstrates that single-event correlations inflate uncertainties in population correlations and that catalog-wide correlated biases can be misread as population correlations.
92% of 91 LIGO black hole mergers favor non-zero V_GW, constraining bound remnants to at most 8% and finding no cosmological handedness preference with average near zero.
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Simulations with a new tidal model in COMPAS predict that merging binary black holes from isolated evolution are strongly biased to low effective spins, with one third below 0.05 and only 3% above 0.5, but the high-spin fraction rises to 15% at higher redshifts.
GWTC-5.0 analysis finds evidence for structure beyond a non-skewed Gaussian bulk in χ_eff, with suggestive mass-dependent excess of positive over negative spins outside the bulk at 13:1 odds in one mass bin.
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.
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When the black holes align: a subpopulation of aligned massive binary black holes observed via gravitational waves
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