RECORD
GW230529_181500: A Potential Primordial Binary Black Hole Merger in the Mass Gap
General Relativity and Quantum Cosmology · Submitted 8 Apr 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim In this paper, we propose that GW230529_181500 originated from the merger of two primordial black holes (PBHs).
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
During the fourth observing run of the LIGO-Virgo-KAGRA detector network, the LIGO Livingston observatory detected a coalescing compact binary, GW230529_181500, with component masses of $2.5-4.5\, M_\odot$ and $1.2-2.0\, M_\odot$ at the $90\%$ credible level. The gravitational-wave data alone is insufficient to determine whether the components are neutron stars or black holes. In this paper, we propose that GW230529_181500 originated from the merger of two primordial black holes (PBHs). We estimate a merger rate of $5.0^{+47.0}_{-4.9} \mathrm{Gpc}^{-3}\,\mathrm{yr}^{-1}$ for compact binary coalescences with properties similar to GW230529_181500. Assuming the source is a PBH-PBH merger, GW230529-like events lead to approximately $1.7^{+36.2}_{-1.5} \times 10^{-3}$ of the dark matter in the form of PBHs. The required abundance of PBHs to explain this event is consistent with existing upper limits derived from microlensing, cosmic microwave background observations and the null detection of gravitational wave background by LIGO-Virgo-KAGRA.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | During the fourth observing run of the LIGO-Virgo-KAGRA detector network, the LIGO Livingston observatory detected a coalescing compact binary, GW230529_181500, with component masses of $2.5-4.5\, M_\odot$ and $1.2-2.0\, M_\odot$ at the $90\%$ credible level. | result 0.94 | 0.75 | 0.05 | asserted 1.00 |
| s1 | The gravitational-wave data alone is insufficient to determine whether the components are neutron stars or black holes. | gap 0.48 | 0.41 | 0.02 | asserted 1.00 |
| s2 | In this paper, we propose that GW230529_181500 originated from the merger of two primordial black holes (PBHs). | contribution 0.67 | 0.81 | 0.73 | speculative 0.72 |
| s3 | We estimate a merger rate of $5.0^{+47.0}_{-4.9} \mathrm{Gpc}^{-3}\,\mathrm{yr}^{-1}$ for compact binary coalescences with properties similar to GW230529_181500. | result 0.99 | 0.94 | 0.07 | asserted 0.94 |
| s4 | Assuming the source is a PBH-PBH merger, GW230529-like events lead to approximately $1.7^{+36.2}_{-1.5} \times 10^{-3}$ of the dark matter in the form of PBHs. | result 0.88 | 0.90 | 0.10 | asserted 0.75 |
| s5 | The required abundance of PBHs to explain this event is consistent with existing upper limits derived from microlensing, cosmic microwave background observations and the null detection of gravitational wave background by LIGO-Virgo-KAGRA. | interpretation 0.77 | 0.37 | 0.15 | hedged possibility 0.83 |
What was examined, and what was not
- arXiv listing abstract v2
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
During the fourth observing run of the LIGO-Virgo-KAGRA detector network, the LIGO Livingston observatory detected a coalescing compact binary, GW230529_181500, with component masses of $2.5-4.5\, M_\odot$ and $1.2-2.0\, M_\odot$ at the $90\%$ credible level. The gravitational-wave data alone is insufficient to determine whether the components are neutron stars or black holes. In this paper, we propose that GW230529_181500 originated from the merger of two primordial black holes (PBHs). We estimate a merger rate of $5.0^{+47.0}_{-4.9} \mathrm{Gpc}^{-3}\,\mathrm{yr}^{-1}$ for compact binary coalescences with properties similar to GW230529_181500. Assuming the source is a PBH-PBH merger, GW230529-like events lead to approximately $1.7^{+36.2}_{-1.5} \times 10^{-3}$ of the dark matter in the form of PBHs. The required abundance of PBHs to explain this event is consistent with existing upper limits derived from microlensing, cosmic microwave background observations and the null detection of gravitational wave background by LIGO-Virgo-KAGRA.
Human review
References
How the literature uses it
15 arXiv papers cite this in 17 sentences
Papers citing it · 14 sentences without a confident label
Cites it as background 3 papers
-
Primordial BHs (PBHs), seeded by the catastrophic gravitational collapse of primordial density fluctuations in the early Universe [ref] , offer a natural and compelling resolution [ref] .
Constraints on the Primordial Black Hole Abundance using Pulsar Parameter Drifts · Introduction · 0.89
-
Complementary GW probes of PBHs include compact binary mergers and the GW signatures during the formation of PBHs [ref] .
Projected Constraints on Primordial Black Holes from Scalar-Induced Gravitational Waves with Taiji · Introduction · 0.83
-
IGWs have emerged as a promising new probe of primordial black holes (PBHs) [ref] , which have garnered significant interest in recent years [ref] due to their potential to explain dark matter [ref] and serve as sources for the gravitational wave events detected by the LIGO-Virgo-KAGRA collaboration [ref] .
Gauge Dependence of Gravitational Waves Induced by Primordial Isocurvature Fluctuations · Introduction · 0.83
What it cites · 32 sentences without a confident label
Uses the method or tool of 12 papers
-
The estimation of $ξ(Λ)$ is performed using simulated injections [ref] , where a Monte Carlo integral over found injections [ref] is used to approximate $ξ(Λ)$ as [equation] with $N_inj$ representing the total number of injections, $N_found$ denoting the count of successfully detected injections, and $p_draw$ being the probability density function from which the injections are drawn.
The population of merging compact binaries inferred using gravitational waves through GWTC-3 · Methodology · 0.93
-
The merger rate density of a PBH binary at cosmic time $t$ is expressed as [ref] [equation] where $t_0$ is the present cosmic time, $M=m_1 + m_2$ is the total mass, $η≡m_1 m_2/M^2$, $f_PBH=Ω_pbh/Ω_m$ is the total fraction of dark matter in PBHs, and the suppression factor $S[P(m), f_PBH, M]$ which is given by Ref. [ref] takes into account the influence of the surrounding smooth matter component on binary formation and the potential disruption of the binary system by PBHs.
Effects of the surrounding primordial black holes on the merger rate of primordial black hole binaries · Merger rate of PBH binaries · 0.88
-
The merger rate density of a PBH binary at cosmic time $t$ is expressed as [ref] [equation] where $t_0$ is the present cosmic time, $M=m_1 + m_2$ is the total mass, $η≡m_1 m_2/M^2$, $f_PBH=Ω_pbh/Ω_m$ is the total fraction of dark matter in PBHs, and the suppression factor $S[P(m), f_PBH, M]$ which is given by Ref. [ref] takes into account the influence of the surrounding smooth matter component on binary formation and the potential disruption of the binary system by PBHs.
Merger Rate Distribution of Primordial-Black-Hole Binaries · Merger rate of PBH binaries · 0.88
Uses data or values from 2 papers
-
In this work, we use the “Combined_PHM_highSpin" posteriors as released by LVK [ref] .
Observation of Gravitational Waves from the Coalescence of a $2.5\text{-}4.5~M_\odot$ Compact Object and a Neutron Star · Methodology · 0.99
-
When converting between luminosity distances, times, and redshifts, we adopt the best-fit cosmological model of Planck 2018 [ref] .
Planck 2018 results. VI. Cosmological parameters · Merger rate of PBH binaries · 0.85
Compares with 10 papers
-
The observational constraints include EROS/MACHO microlensing [ref] , OGLE microlensing [ref] , stochastic GW background (SGWB) from binary PBHs [ref] and accretion constraints of cosmic microwave background (CMB) [ref] .
Constraint on the abundance of primordial black holes in dark matter from Planck data · Result and discussion · 0.95
-
The observational constraints include EROS/MACHO microlensing [ref] , OGLE microlensing [ref] , stochastic GW background (SGWB) from binary PBHs [ref] and accretion constraints of cosmic microwave background (CMB) [ref] .
Constraints on the Primordial Black Hole Abundance from the First Advanced LIGO Observation Run Using the Stochastic Gravitational-Wave Background · Result and discussion · 0.95
-
The observational constraints include EROS/MACHO microlensing [ref] , OGLE microlensing [ref] , stochastic GW background (SGWB) from binary PBHs [ref] and accretion constraints of cosmic microwave background (CMB) [ref] .
Cosmic microwave background limits on accreting primordial black holes · Result and discussion · 0.95
Cites as support 1 paper
-
Secondly, given that the merger rate of PBH-NS mergers is much lower than a PBH-PBH merger [ref] , this leaves us with the intriguing possibility that we might observe phenomena involving the PBH-PBH merger.
Establishing the Non-Primordial Origin of Black Hole-Neutron Star Mergers · Result and discussion · 0.98
Cites as background 25 papers
-
PBHs can form binaries through several formation channels [ref] .
Did LIGO detect dark matter? · Merger rate of PBH binaries · 0.91
-
PBHs can form binaries through several formation channels [ref] .
Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914 · Merger rate of PBH binaries · 0.91
-
PBHs can form binaries through several formation channels [ref] .
Redshift evolution of primordial black hole merger rate · Merger rate of PBH binaries · 0.91
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.