A 4.46 solar-mass black hole is found in a 94-year eccentric orbit with a main-sequence turnoff star in ω Centauri via 23-year astrometric monitoring.
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12 Pith papers cite this work, alongside 380 external citations. Polarity classification is still indexing.
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Milky Way globular clusters formed with initial half-mass densities of ~10^6.4 M_sun/pc^3, bottom-light IMFs, and small present-day black hole mass fractions, inferred by coupling rapid evolution models with multimass equilibrium models fitted to present-day observations.
Hierarchical Bayesian analysis of GWTC-5.0 data identifies a mass transition at 15.2 solar masses separating distinct effective-spin distributions, pointing to different formation channels for low-mass binary black holes.
N-body simulations demonstrate runaway GW BBH mergers in dense BH clusters (≥5×10^9 M⊙/pc³) produce ~10³ M⊙ IMBHs within 10 Myr.
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.
Efficient mass transfer in binaries naturally limits the mass of the first-born black hole and produces a sharp drop above 45 solar masses that mimics the pair-instability gap.
GWTC-4 data analysis yields a pair-instability mass gap lower edge at 44.3^{+5.9}_{-3.5} M_⊙, an S-factor of 268^{+195}_{-116} keV b for ^{12}C(α,γ)^{16}O, and two populations supporting both direct formation and hierarchical mergers.
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.
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.
LILA can detect IMBH binaries at redshifts 20-30, IMRIs, and provide months-to-years early warnings with high-SNR events for gravity tests.
N-body models of young and old dense star clusters show BBH mergers span primary masses from ~6 to >100 solar masses with a peak near 8 solar masses, reproducing the LIGO-inferred distribution, with low-mass mergers mostly from metal-rich clusters.
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.
citing papers explorer
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A Long Period Stellar-Mass Black Hole Binary in $\omega$ Centauri
A 4.46 solar-mass black hole is found in a 94-year eccentric orbit with a main-sequence turnoff star in ω Centauri via 23-year astrometric monitoring.
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Fast Dynamical Modelling of Milky Way Globular Clusters -- I. Implications for Initial Cluster Densities
Milky Way globular clusters formed with initial half-mass densities of ~10^6.4 M_sun/pc^3, bottom-light IMFs, and small present-day black hole mass fractions, inferred by coupling rapid evolution models with multimass equilibrium models fitted to present-day observations.
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Distinct spin properties and astrophysical origin of low mass binary black holes in gravitational wave data
Hierarchical Bayesian analysis of GWTC-5.0 data identifies a mass transition at 15.2 solar masses separating distinct effective-spin distributions, pointing to different formation channels for low-mass binary black holes.
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Rapid intermediate-mass black hole formation via runaway mergers of black holes
N-body simulations demonstrate runaway GW BBH mergers in dense BH clusters (≥5×10^9 M⊙/pc³) produce ~10³ M⊙ IMBHs within 10 Myr.
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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.
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Binary Evolution Can Mimic the Pair-Instability Mass Gap in Black Hole Mergers
Efficient mass transfer in binaries naturally limits the mass of the first-born black hole and produces a sharp drop above 45 solar masses that mimics the pair-instability gap.
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Gravitational-wave constraints on the pair-instability mass gap and nuclear burning in massive stars
GWTC-4 data analysis yields a pair-instability mass gap lower edge at 44.3^{+5.9}_{-3.5} M_⊙, an S-factor of 268^{+195}_{-116} keV b for ^{12}C(α,γ)^{16}O, and two populations supporting both direct formation and hierarchical mergers.
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Intrinsic handedness in O1-O4a black-hole mergers: probing orbital precession, remnant retention in dense environments and cosmological mirror asymmetry
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.
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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.
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Black Hole Binary Detection Landscape for the Laser Interferometer Lunar Antenna (LILA): Signal-to-Noise Calculations & Science Cases
LILA can detect IMBH binaries at redshifts 20-30, IMRIs, and provide months-to-years early warnings with high-SNR events for gravity tests.
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Mass Distribution of Binary Black Hole Mergers from Young and Old Dense Star Clusters
N-body models of young and old dense star clusters show BBH mergers span primary masses from ~6 to >100 solar masses with a peak near 8 solar masses, reproducing the LIGO-inferred distribution, with low-mass mergers mostly from metal-rich clusters.
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McFACTS II: Mass Ratio--Effective Spin Relationship of Black Hole Mergers in the AGN Channel
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.