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.
The SXS Collaboration catalog of binary black hole simulations
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Derives large-eccentricity asymptotics for post-Newtonian eccentric waveform Fourier modes and builds a fast endpoint-constrained analytic approximation with error under 10^{-3} valid to p=200.
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.
FIREFLY accelerates multi-mode GW ringdown analysis by analytically marginalizing QNM amplitudes and phases via Bayesian principles and importance sampling.
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.
Extended-data Bayesian reanalysis of GW190814 finds no evidence for tertiary-induced line-of-sight acceleration or residual eccentricity due to strong degeneracy between the two effects.
citing papers explorer
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GW231123: a Binary Black Hole Merger with Total Mass 190-265 $M_{\odot}$
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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On the Presence of a Tertiary Compact Object in GW190814
Extended-data Bayesian reanalysis of GW190814 finds no evidence for tertiary-induced line-of-sight acceleration or residual eccentricity due to strong degeneracy between the two effects.