A new gravitational wave event reveals a binary black hole merger with total mass 190-265 solar masses, indicating black holes can form via gravitational-wave driven mergers beyond standard stellar channels.
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N-body simulations demonstrate runaway GW BBH mergers in dense BH clusters (≥5×10^9 M⊙/pc³) produce ~10³ M⊙ IMBHs within 10 Myr.
Eccentricity posteriors of dynamically captured binaries can be mapped to capture parameters and compared against environment velocity distributions to constrain host and infer decay time.
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.
Ground-triggered Bayesian analysis enables detection and tight constraints on eccentricity and chirp mass for a GW190521-like eccentric binary black hole in one year of LISA or TianQin data at SNR ~7.
Updated ANC constraints on the 12C(alpha,gamma)16O S-factor favor lower values than prior evaluations and imply a black-hole mass-gap lower edge of 61-75 solar masses.
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.
Isolated Population III binaries can form GW231123-like events if convective overshooting is inefficient, the carbon-alpha reaction rate is 2 sigma below standard, and initial orbits match those of later-generation binaries.
Monte Carlo simulations of AGN-disk black hole mergers identify dense, moderately short-lived disks, a steep initial mass function, and mostly prograde orbits as the parameter combination that reproduces the observed (q, χ_eff) anti-correlation.
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.
Simulations show LIGO-A# constrains the peak redshift of binary black hole merger rate (tracing star formation) to ±0.1 in one year, improving to ±0.02 with next-generation detectors.
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.
LIGO-Virgo-KAGRA releases calibrated strain time series, noise-subtraction channels, and GWOSC v5.0 analysis products covering April 2024 to January 2025.
The paper computes the graviton-scalar Compton scattering cross section via EFT at ~30 PeV center-of-mass energy and derives an impact parameter that, after coherence enhancement, scales with the known LIGO GW strain and mirror recoil.
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