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Constraining the origin of stellar binary black hole mergers by detections of their lensed host galaxies and gravitational wave signals
High Energy Astrophysical Phenomena · Submitted 18 Oct 2022
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Therefore, with the third generation GW detectors and future large scale galaxy surveys, it is possible to independently constrain the sBBH origin via the detection fraction of those lensed events with identifiable lensing host signatures and/or even constrain the contribution fractions from different sBBH formation mechanisms
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The abstract, sentence by sentence
A significant number of stellar binary black hole (sBBH) mergers may be lensed and detected by the third generation gravitational wave (GW) detectors. Their lensed host galaxies may be detectable, which thus helps to accurately localize these sources and provide a new approach to study the origin of sBBHs. In this paper, we investigate the detectability of the lensed host galaxies for the lensed sBBH mergers. We find that the detection fraction of the host galaxies to the lensed GW events can be significantly different for a survey with a given limiting magnitude if sBBHs are produced by different mechanisms, such as the evolution of massive binary stars, the dynamical interactions in dense star clusters, and that assisted by active galactic nuclei or massive black holes. Furthermore, we illustrate that the statistical spatial distribution of those lensed sBBHs in its hosts resulting from different sBBH formation channels can be different from each other. Therefore, with the third generation GW detectors and future large scale galaxy surveys, it is possible to independently constrain the sBBH origin via the detection fraction of those lensed events with identifiable lensing host signatures and/or even constrain the contribution fractions from different sBBH formation mechanisms
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | A significant number of stellar binary black hole (sBBH) mergers may be lensed and detected by the third generation gravitational wave (GW) detectors. | background 1.00 | 0.08 | 0.04 | hedged possibility 1.00 |
| s1 | Their lensed host galaxies may be detectable, which thus helps to accurately localize these sources and provide a new approach to study the origin of sBBHs. | background 0.89 | 0.07 | 0.08 | hedged possibility 0.99 |
| s2 | In this paper, we investigate the detectability of the lensed host galaxies for the lensed sBBH mergers. | contribution 1.00 | 0.61 | 0.03 | asserted 0.90 |
| s3 | We find that the detection fraction of the host galaxies to the lensed GW events can be significantly different for a survey with a given limiting magnitude if sBBHs are produced by different mechanisms, such as the evolution of massive binary stars, the dynamical interactions in dense star clusters, and that assisted by active galactic nuclei or massive black holes. | result 1.00 | 0.94 | 0.19 | asserted 1.00 |
| s4 | Furthermore, we illustrate that the statistical spatial distribution of those lensed sBBHs in its hosts resulting from different sBBH formation channels can be different from each other. | result 1.00 | 0.84 | 0.08 | asserted 0.92 |
| s5 | Therefore, with the third generation GW detectors and future large scale galaxy surveys, it is possible to independently constrain the sBBH origin via the detection fraction of those lensed events with identifiable lensing host signatures and/or even constrain the contribution fractions from different sBBH formation mechanisms | interpretation 0.97 | 0.24 | 0.91 | hedged possibility 0.99 |
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Original abstract
A significant number of stellar binary black hole (sBBH) mergers may be lensed and detected by the third generation gravitational wave (GW) detectors. Their lensed host galaxies may be detectable, which thus helps to accurately localize these sources and provide a new approach to study the origin of sBBHs. In this paper, we investigate the detectability of the lensed host galaxies for the lensed sBBH mergers. We find that the detection fraction of the host galaxies to the lensed GW events can be significantly different for a survey with a given limiting magnitude if sBBHs are produced by different mechanisms, such as the evolution of massive binary stars, the dynamical interactions in dense star clusters, and that assisted by active galactic nuclei or massive black holes. Furthermore, we illustrate that the statistical spatial distribution of those lensed sBBHs in its hosts resulting from different sBBH formation channels can be different from each other. Therefore, with the third generation GW detectors and future large scale galaxy surveys, it is possible to independently constrain the sBBH origin via the detection fraction of those lensed events with identifiable lensing host signatures and/or even constrain the contribution fractions from different sBBH formation mechanisms
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References
How the literature uses it
3 arXiv papers cite this in 3 sentences
Papers citing it · 1 sentence without a confident label
Uses its data or values 1 paper
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However, for the prediction of future specific telescopes, [ref] and [ref] estimated that the fraction of those lensed galaxies detected by sky surveys (e,g,, Euclid, CSST, etc.) is about $20-50%$.
On the detection of the electromagnetic counterparts from lensed gravitational wave events by binary neutron star mergers · Joint detection of lensed GW+EM events · 0.86
Compares with it 1 paper
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Here, we generate mock BBHs for millihertz and decihertz GW detectors which is different from the method for generating mock samples in hectohertz detectors as in the work by [ref] .
Multiband gravitational wave observations of stellar binary black holes at the low to middle and high frequencies · Mock Sample of BBHs · 0.87
What it cites · 13 sentences without a confident label
Uses the method or tool of 2 papers
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The localization error for each sBBH GW source may be estimated according to the Fisher information matrix [ref] , $Γ_jk$, which is defined as
Detectability and parameter estimation of stellar origin black hole binaries with next generation gravitational wave detectors · Samplings and Criteria · 0.99
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The localization error for each sBBH GW source may be estimated according to the Fisher information matrix [ref] , $Γ_jk$, which is defined as
Forecasting the detection capabilities of third-generation gravitational-wave detectors using $\texttt{GWFAST}$ · Samplings and Criteria · 0.99
Uses data or values from 2 papers
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Therefore, as estimated by [ref] , the above predicted rate may be reduced by at most a factor of $∼0.35-0.20$ due to this localization error of the GW signals ($1-5$ deg$^2$) and reconstruction errors for the lensed host galaxies.
On the detection and precise localisation of merging black holes events through strong gravitational lensing · Results · 0.85
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3) The image and counter-image must be resolvable, i.e., $R_e^2+s^2/2≲θ_E^2$, where $s$ is the seeing, e.g., $0.18^''$ for the i-band of CSST [ref] , $0.23^''$ for the VIS-band of Euclid [ref] and $0.11^''$ for the J-band of RST [ref] .
Wide-Field InfraRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA Final Report · Samplings and Criteria · 0.96
Compares with 1 paper
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Noticed that, the above criteria is relatively stricter than those adopted in [ref] , even though the criteria for identifying a lensed host themselves are quite flexible.
On the detection and precise localisation of merging black holes events through strong gravitational lensing · Samplings and Criteria · 1.00
Cites as background 1 paper
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These sBBHs can be originated from (1) the evolution of massive binary stars [ref] , (2) the dynamical interactions in dense stellar systems [ref] , or (3) the active galactic nuclei (AGN) or massive black hole (MBH) assisted mechanisms [ref] .
Blackhole Mergers Through Evection Resonances · Introduction · 0.94
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