Demonstrates direct comparison of observable compact-binary populations from GW data to astrophysical models, with unbiased inference shown possible and applied to O3 data.
Merging black hole binaries: the effects of progenitor's metallicity, mass-loss rate and Eddington factor
5 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The first four gravitational wave events detected by LIGO were all interpreted as merging black hole binaries (BHBs), opening a new perspective on the study of such systems. Here we use our new population-synthesis code MOBSE, an upgraded version of BSE (Hurley et al. 2002), to investigate the demography of merging BHBs. MOBSE includes metallicity-dependent prescriptions for mass loss of massive hot stars. It also accounts for the impact of the electron-scattering Eddington factor on mass loss. We perform >10^8 simulations of isolated massive binaries, with 12 different metallicities, to study the impact of mass loss, core-collapse supernovae and common envelope on merging BHBs. Accounting for the dependence of stellar winds on the Eddington factor leads to the formation of black holes (BHs) with mass up to 65 Msun at metallicity Z~0.0002. However, most BHs in merging BHBs have masses <40 Msun. We find merging BHBs with mass ratios in the 0.1 - 1.0 range, even if mass ratios >0.6 are more likely. We predict that systems like GW150914, GW170814 and GW170104 can form only from progenitors with metallicity Z<=0.006, Z<=0.008 and Z<=0.012, respectively. Most merging BHBs have gone through a common envelope phase, but up to ~17 per cent merging BHBs at low metallicity did not undergo any common envelope phase. We find a much higher number of mergers from metal-poor progenitors than from metal-rich ones: the number of BHB mergers per unit mass is ~10^-4 Msun^-1 at low metallicity (Z = 0.0002 - 0.002) and drops to ~10^-7 Msun^-1 at high metallicity (Z ~ 0.02).
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An isolated hierarchical triple channel with chemically homogeneous evolution and triple common envelope can produce PISN mass-gap BBH mergers matching GW190706 at ~22% of the observed rate.
Slowly rotating 80–85 M☉ Pop III stars can keep most of their mass and form black holes with spins up to a_BH ≲ 0.7 just below the pair-instability gap.
Introduces a target redshift z_t to isolate metal-poor black hole progenitors and a statistical framework to test merger-rate variations against forecasts from Einstein Telescope and Cosmic Explorer.
The paper evaluates how triangular versus two-L-shaped geometries, arm lengths, and presence of low-frequency instruments affect the science reach of the Einstein Telescope for compact binaries, multi-messenger events, and stochastic backgrounds.
citing papers explorer
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Comparing astrophysical models to gravitational-wave data in the observable space
Demonstrates direct comparison of observable compact-binary populations from GW data to astrophysical models, with unbiased inference shown possible and applied to O3 data.
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A Possible Triple Formation Scenario of Binary Black Hole Merge With One In Pair-instability Supernova Mass Gap
An isolated hierarchical triple channel with chemically homogeneous evolution and triple common envelope can produce PISN mass-gap BBH mergers matching GW190706 at ~22% of the observed rate.
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Fast-spinning massive black holes from slowly rotating low-metallicity stars: Implications for GW231123
Slowly rotating 80–85 M☉ Pop III stars can keep most of their mass and form black holes with spins up to a_BH ≲ 0.7 just below the pair-instability gap.
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Targeting black holes from metal-poor progenitors with next-generation gravitational-wave detectors
Introduces a target redshift z_t to isolate metal-poor black hole progenitors and a statistical framework to test merger-rate variations against forecasts from Einstein Telescope and Cosmic Explorer.
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Science with the Einstein Telescope: a comparison of different designs
The paper evaluates how triangular versus two-L-shaped geometries, arm lengths, and presence of low-frequency instruments affect the science reach of the Einstein Telescope for compact binaries, multi-messenger events, and stochastic backgrounds.