Optimal SSB frame origin for LGWA cuts sampling time by 10x and tightens chirp mass and sky position constraints for stellar-mass binaries beyond LVK performance.
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A new redshift-correlation technique with third-generation GW detectors can constrain the BNS contribution to cosmic r-process nucleosynthesis to 5-6% precision via Fisher forecasts on mock bright- and dark-siren data.
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.
Bayesian analysis of LISA EMRIs in AGN disks constrains disk surface density and accretion rate to ~10% using relativistic torque models, invalidating Fisher-matrix forecasts and enabling dark-siren cosmology without EM counterparts.
N-body simulations demonstrate runaway GW BBH mergers in dense BH clusters (≥5×10^9 M⊙/pc³) produce ~10³ M⊙ IMBHs within 10 Myr.
Two FRBs exhibit microlensing signatures consistent with intermediate-mass black holes of masses approximately 500-600 and 1500-2500 solar masses, interpreted as possible evidence for isolated primordial black holes comprising about 4% of dark matter.
Black hole merger properties in AGN disks match observed distributions when gas accretion and hierarchical mergers are included, varying strongly with disk parameters.
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.
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.
Coupled cosmological and cluster simulations show isolated binary evolution cannot produce GW231123-like mergers at the observed redshift, while hierarchical mergers in globular clusters can, yielding a local rate of 0.78 Gpc^{-3} yr^{-1} peaking at z=4-6.
Stellar models show that the 12C(alpha,gamma)16O rate uncertainty moves the black hole mass gap, constraining its S300 to 137.6-263.4 keV barn when matched to the observed gap from gravitational waves.
Reanalysis of GW231123 shows no significant eccentricity, with parameter estimate differences explained by waveform model disagreements at strong spin precession.
Some opacity in black hole imaging methods is compatible with reliable inference under specified conditions, but GRMHD models of Sgr A* exhibit problematic opacity that signals model limitations.
High-metallicity star cluster simulations produce black hole mergers with masses and ratios consistent with recent LVK detections, unlike low-metallicity models.
Simulations show VMS in star clusters reach 10^3-10^4 solar masses with dimensionless spins >10 under bloated accretion conditions, potentially forming spinning IMBHs that produce GW bursts like GW190521.
Modeling of jets escaping AGN disks reveals distinct nonthermal emission signatures that support multi-messenger detection and diagnostics of the AGN environment.
Describes the methods for producing the fifth gravitational-wave transient catalog (GWTC-5.0) from O4b data of LIGO, Virgo and KAGRA.
LIGO-Virgo-KAGRA releases calibrated strain time series, noise-subtraction channels, and GWOSC v5.0 analysis products covering April 2024 to January 2025.
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