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.
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Reversible-jump MCMC analysis of LIGO binary black hole mergers identifies three subpopulations with distinct properties and independent redshift evolution.
Simulations find nested bow shocks around an engulfed neutron star enhance drag force 10-100 times over Bondi-Hoyle-Lyttleton and allow force reversal based on envelope conditions.
A parametrized analytical model for BBH mass ratios from the stable mass transfer channel is derived and applied to the 10 solar-mass peak in GWTC-4, favoring little mass-ratio reversal.
Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.
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.
GWTC-5 chirp-mass peaks form a ~1.9-spaced ladder with a new ~19 M⊙ rung matching predicted 2G+3G mergers, unifying prior 1G+2G spin-transition groups under one hierarchical scenario.
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
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.
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.
Simulations with a new tidal model in COMPAS predict that merging binary black holes from isolated evolution are strongly biased to low effective spins, with one third below 0.05 and only 3% above 0.5, but the high-spin fraction rises to 15% at higher redshifts.
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.
A decade of gravitational-wave data shows most merging stellar-mass black holes have small spins, with subdominant fast-spinning, misaligned, and hierarchical-merger populations.
citing papers explorer
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The First Detection of Sub-Populations in the Delay-Time Distribution of Binary Black Holes in GWTC-4 of LIGO-Virgo-KAGRA
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.
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Reversible-jump MCMC reveals binary black hole subpopulations with distinct redshift evolution
Reversible-jump MCMC analysis of LIGO binary black hole mergers identifies three subpopulations with distinct properties and independent redshift evolution.
-
Numerical Studies of Accretion Flows onto a Neutron Star Engulfed in a Massive Star
Simulations find nested bow shocks around an engulfed neutron star enhance drag force 10-100 times over Bondi-Hoyle-Lyttleton and allow force reversal based on envelope conditions.
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A Strongly Parametrized Mass Ratio Model for the Stable Mass Transfer Channel: a Case Study of the $10 \, \rm{M}_{\odot}$ Peak
A parametrized analytical model for BBH mass ratios from the stable mass transfer channel is derived and applied to the 10 solar-mass peak in GWTC-4, favoring little mass-ratio reversal.
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Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions
Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.
-
Forbidden Formation Histories: The Binary Black Hole Merger Rate Disfavors Long Delay Times
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.
-
The Chirp-Mass Ladder: A New Rung Emerges
GWTC-5 chirp-mass peaks form a ~1.9-spaced ladder with a new ~19 M⊙ rung matching predicted 2G+3G mergers, unifying prior 1G+2G spin-transition groups under one hierarchical scenario.
-
AGN-driven BBH mergers: Black hole populations and hierarchical growth across the AGN parameter space
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
-
Compactness Peaks and Subpopulations: Probing Stellar Physics and Formation Channels of Merging Binary Black Holes
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.
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How do the LIGO-Virgo-KAGRA's Heavy Black Holes Form? No evidence for core-collapse Intermediate-mass black holes in GWTC-4
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.
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Where are Gaia's small black holes?
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.
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Modern tidal interaction models for rapid binary population synthesis: II. Binary black hole formation, mergers, and spins
Simulations with a new tidal model in COMPAS predict that merging binary black holes from isolated evolution are strongly biased to low effective spins, with one third below 0.05 and only 3% above 0.5, but the high-spin fraction rises to 15% at higher redshifts.
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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.
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The first decade of gravitational-wave measurements of black hole spins
A decade of gravitational-wave data shows most merging stellar-mass black holes have small spins, with subdominant fast-spinning, misaligned, and hierarchical-merger populations.