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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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.
Statistical combination of sub-threshold post-merger signals from 50-70 BNS events can constrain the maximum mass of hot neutron stars to 11-20% fractional uncertainty, potentially translating to 12-21% on the cold TOV mass.
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.
Gravitational wave remnants from GWTC-4.0 binary mergers are consistent with general relativity Kerr black hole predictions, with no evidence for post-merger echoes.
Describes the methods for producing the fifth gravitational-wave transient catalog (GWTC-5.0) from O4b data of LIGO, Virgo and KAGRA.
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GWTC-5.0: Observations from the Second Part of the Fourth LIGO-Virgo-KAGRA Observing Run and Updates to the Gravitational-Wave Transient Catalog
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-4.0: Tests of General Relativity. III. Tests of the Remnants
Gravitational wave remnants from GWTC-4.0 binary mergers are consistent with general relativity Kerr black hole predictions, with no evidence for post-merger echoes.
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GWTC-5.0: Methods for Identifying and Characterizing Gravitational-wave Transients
Describes the methods for producing the fifth gravitational-wave transient catalog (GWTC-5.0) from O4b data of LIGO, Virgo and KAGRA.