GWTC-5.0 adds 161 new compact binary coalescence candidates from O4b with p_astro >= 0.5, detailed properties for 104, all binary black holes, for a cumulative total of 390.
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GWTC-4 data reveals three sub-populations of binary black holes with distinct delay-time distributions that depend on mass above 45 solar masses, mass-ratio, and spin, ruling out a single universal merger rate.
Massive black hole binary mergers produce orphaned low-frequency signals in PTA pulsar terms that can be stacked for archival multiband gravitational-wave detection.
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.
Detection of GW190814 from the coalescence of a 23 solar-mass black hole and a 2.6 solar-mass compact object, the most unequal-mass binary yet observed with gravitational waves.
Deconvolution of the GWTC-4.0 BBH merger rate reveals that long-delay tails in the delay time distribution are forbidden, constraining progenitor formation histories to decline more steeply than the star formation rate and disfavoring shallow power-law DTDs such as stable mass transfer.
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.
Mixture model analysis of LIGO data identifies a ~10% high-spin subpopulation with a1 ≈ 0.9 matching AGN accretion predictions, disfavoring hierarchical mergers at a1 ≈ 0.7 for that group.
Hierarchical Bayesian inference allows accurate recovery of intrinsic astrophysical source populations even when follow-up selection is unknown and correlated with parameters of interest.
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.
FluxMC integrates flow matching with parallel tempering MCMC to converge in under five hours on high-fidelity IMRPhenomHM waveforms for massive black hole binaries, where standard methods fail after hundreds of hours and produce two to three orders of magnitude higher distributional error.
A Gaussian process framework with a localized-deviation kernel is used to test general relativity on simulated and GWTC-3 binary black hole signals, finding no evidence for deviations and limiting strain deviations to 7% for one event.
Score-based diffusion models learn the empirical distribution of real LIGO noise to enable unbiased gravitational-wave parameter estimation under only an additivity assumption.
Introduces a frequentist p-value approach to falsify models of binary black hole formation for events such as GW190521, showing some models are adequate while others are not.
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.
Statistical framework ranks candidate frequencies by combined amplitude and phase uncertainty widths from empirical percentiles, selecting 244 Hz for KAGRA sensing calibration with reduced amplitude interval width.
BBH-Genesis applied to GWTC-4 finds strongest support for a two-channel model of binary black hole populations with possible mild evidence for an AGN-related third channel.
A stripped-star-motivated five-component model for binary black hole populations is preferred over the LVK baseline by a log10 Bayes factor of 7.69 and attributes the observed mass features to isolated, dynamical, and hierarchical formation channels.
No evidence for core-collapse formed low-spin IMBHs in GWTC-4, with 90% upper limit on merger rate of 0.077 Gpc^{-3} yr^{-1}, low-spin BH mass truncation at 65 solar masses consistent with pair-instability gap lower edge, and high-spin IMBHs from hierarchical mergers.
Self-lensing signals occur with probabilities of roughly 10^{-3} in WD+NS systems and 10^{-2} in WD+BH systems; TESS could detect at least one if 8% of white dwarfs have NS companions and 3% have BH companions, while Roman cannot.
Natal kicks from supernovae are proposed to disrupt Gaia progenitor binaries containing low-mass black holes more frequently than those leading to gravitational-wave mergers, accounting for the observed difference in the 2.5-5 solar mass gap.
A targeted gravitational-wave search modifies the GstLAL likelihood ratio with a sky localization prior from EM triggers, showing improved detection efficiency in injection studies while controlling false alarms.
An analytical model for core-bounce gravitational waveforms estimates the rotation parameter β with 94% average fitting factor to numerical templates and derives error bounds below 0.1 via matched filtering and Cramér-Rao comparison in O4 noise at 5-50 kpc distances.
MUST is a new 6.5 m telescope designed to deliver simultaneous optical spectra for over 20,000 targets across a 5 deg² field, enabling the largest 3D spectroscopic map of the Universe with redshifts for more than 100 million objects over an 8-year survey.
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