Pith. sign in

REVIEW 2 major objections 4 minor 2 cited by

Search for a gravitational wave background from primordial black hole binaries using data from the first three LIGO-Virgo-KAGRA observing runs

T0 review · 2 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read A Bayesian search of the first three observing runs finds no primordial black hole background and sets 95% upper limits that largely exclude PBH dark matter from 10 to 300 solar masses.

desk verdict Solid Bayesian stochastic-search paper with a real caveat: the headline f_PBH limits rely on suppression formulas the authors themselves flag as unvalidated for broad mass distributions, so the constraints are model-conditional, not absolute dark-matter exclusions. read the letter →

arxiv 2412.18318 v3 pith:HL5T6HXJ submitted 2024-12-24 astro-ph.CO gr-qc

Tore Boybeyi , Sebastien Clesse , Sachiko Kuroyanagi , Mairi Sakellariadou This is my paper · ORCID
classification astro-ph.COgr-qc
keywords gravitationalwavebackgroundprimordialblackholesstochasticdarkmatterconstraintsBayesianinferencebinaryholemergerslog-normalmassfunctionearlyandlateformation
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

Using the cross-correlation data from the first three observing runs of the ground-based gravitational-wave detector network, this paper searches for a gravitational-wave background (GWB) produced by binaries of primordial black holes (PBHs), modelling both early- and late-formation channels and a log-normal mass function. No such background is found, and the null result is converted into 95% upper limits on the fraction $f_{\rm PBH}$ of dark matter in PBHs as a function of mean mass. At 30 solar masses the limit reaches $f_{\rm PBH} < 5.3\times10^{-3}$ (for a reference clustering parameter $R_{\rm clust}=1$), and the constraints improve previous GWB-based bounds by a factor of about 2–10 at 100 solar masses. If correct, these limits strengthen the case that PBHs do not constitute all of the dark matter in the roughly 10–300 solar mass window.

What carries the argument

The central object is the isotropic gravitational-wave background model $\Omega_{\rm GW}(f) = \Omega_{\rm CBC}(f) + \Omega_{\rm EB}(f) + \Omega_{\rm LB}(f)$, where $\Omega_{\rm CBC}$ is a fiducial astrophysical compact-binary (CBC) power-law background and $\Omega_{\rm EB}$ and $\Omega_{\rm LB}$ are the early- and late-binary PBH contributions computed from the differential merger rates in Eqs. (5) and (6). The early-binary rate carries suppression factors $S_1$ and $S_2$ for matter inhomogeneities and Poisson clustering, while the late-binary rate is scaled by a clustering parameter $R_{\rm clust}$. This spectral shape is compared with the cross-correlation estimator from all available detector baselines through a Gaussian likelihood, and Bayesian nested sampling provides posterior distributions and 95% upper limits on $f_{\rm PBH}$, $\sigma$, $\mu$, and $\Omega_{\rm CBC}$.

What would settle it

Recompute the 95% upper limits using merger rates calibrated to a large $N$-body simulation of PBH binary formation that includes cluster disruption and accretion; if the resulting limits on $f_{\rm PBH}$ are weaker than the quoted values (e.g., $f_{\rm PBH}<5.3\times10^{-3}$ at $30\,M_\odot$), the rate normalization behind the central claim is falsified. Alternatively, a future detector measurement of a PBH GWB below the predicted amplitude for $f_{\rm PBH}=1$ would show the formulas over-predict the background.

Watch

Extended reading notes

Core claim

The paper's central claim is that, under a log-normal PBH mass distribution with width $\sigma<1$ and the standard early/late binary merger-rate prescriptions, the absence of a detectable PBH gravitational-wave background in the first three observing runs rules out $f_{\rm PBH}$ values above roughly $10^{-2}$--$10^{-3}$ for mean masses around 30 solar masses and provides upper limits that improve earlier stochastic-background constraints by a factor of 2–10 at 100 solar masses. The limit is obtained by a full Bayesian fit to the shape of the cross-correlation spectrum rather than by comparing a single power-law bound to a predicted amplitude, and the paper states that this is the first direct GWB search specifically targeting PBH mergers.

Load-bearing premise

The load-bearing premise is that the early- and late-binary merger-rate formulas (Eqs. (5) and (6), with the Appendix A suppression factors) correctly describe how many PBH mergers produce a given $f_{\rm PBH}$; if the true rates are lower, every quoted upper limit on $f_{\rm PBH}$ is too strong, and the paper itself cautions that claims based on these rates may be premature.

Editorial extensions

If this is right

  • If the central claim is correct, PBHs with a narrow log-normal mass distribution cannot make up all of the dark matter for mean masses in the roughly 10–300 $M_\odot$ range.
  • The late-binary formation channel dominates the GWB for mean masses above about $3\times10^2\,M_\odot$, so future low-frequency gravitational-wave detectors could extend the $f_{\rm PBH}$ constraints to heavier PBHs.
  • The full-spectrum Bayesian approach improves previous power-law-based GWB constraints on $f_{\rm PBH}$ by a factor of about 2–10 at $100\,M_\odot$.
  • The posteriors show no significant PBH or CBC background, so the data are consistent with noise, with logarithmic Bayes factors near $-1$.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The reliability of the quoted upper limits rests on the merger-rate formulas; if updated $N$-body simulations show that early binaries are disrupted more easily than the $S_1S_2$ prescription encodes, all $f_{\rm PBH}$ limits would become weaker.
  • The same pipeline could be applied to broad mass functions, such as the QCD phase-transition peak, once their merger rates are better understood; the paper explicitly leaves this to future work.
  • A future positive detection of a GWB whose spectrum deviates from a power law in the way PBH models predict would let this method distinguish primordial from astrophysical binaries, rather than merely set upper limits.
  • Because the late-binary contribution depends on the clustering parameter $R_{\rm clust}$ and dominates at high masses, GWB searches of this type could also constrain PBH clustering, not just PBH abundance.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 4 minor

Summary. The paper searches for a gravitational-wave background (GWB) from primordial black hole (PBH) binaries using the public LIGO-Virgo-KAGRA O1-O3 cross-correlation data. The signal model includes early binaries formed in radiation domination and late binaries formed by dynamical capture, with a log-normal PBH mass function and an additional astrophysical CBC power-law component. The authors perform a Bayesian analysis, find no significant signal (log Bayes factors ~ -1), and derive 95% upper limits on the PBH dark-matter fraction f_PBH as a function of the mean mass µ, marginalizing over the width σ and the CBC amplitude; for example, f_PBH < 5.3e-3 at µ = 30 M_sun for R_clust = 1. They claim their results improve previous GWB constraints by a factor of 2-10 at 100 M_sun.

Significance. If the quoted bounds are robust, they strengthen the exclusion of PBH dark matter in the roughly 10-300 M_sun mass range using the stochastic background rather than resolved events, and the paper demonstrates a useful full-spectral-shape approach that goes beyond the power-law upper limits usually reported by the LVK. The statistical machinery is standard, the likelihood and data handling follow well-established pygwb procedures, and the injection study in Appendix C is a welcome validation exercise. However, the quantitative bounds rest on the early-binary merger-rate formulas whose suppression factors are acknowledged by the authors themselves to be unvalidated for the broad mass distributions included in their prior; this limits the certainty of the headline numbers and the quoted improvement over previous work.

major comments (2)
  1. [Appendix A and Sec. II] The analysis marginalizes over σ up to 1 (Table I), yet the early-binary suppression factors S1 and S2 in Eqs. (9)-(14) are, as the authors state in Appendix A, only valid for narrow mass distributions: 'the validity of the above expressions for a broad mass distribution necessitates detailed analytical investigation or validation through N-body simulations,' and 'making claims based on these merging rates may be premature.' Since σ is essentially unconstrained by the data (flat posterior, Figs. 4-6), the quoted limits in Table II and Fig. 1 include models for which the predicted merger rate—and hence the mapping from non-detection to f_PBH—is not reliable. For σ = 1 the mass function spans decades in mass and <m^2>/<m>^2 = e ≈ 2.7, moving substantially away from the narrow-distribution limit, so the suppression factors can be materially different. This is load-bearing because the f_PBH bounds scale inversely with the assumed merger rate; if broad-distribution suppression is stronger than Eqs. (9)-(14) predict, the limits would be too stringent. Please either restrict the analysis to the validated narrow-σ regime (with a clear statement of what 'narrow' means) or provide N-body/analytic validation of the suppression factors for the full prior range.
  2. [Appendix C and Appendix D] The injection study in Appendix C shows that σ and R_clust are not well recovered, and the corner plots in Appendix D confirm an essentially flat posterior for σ. Because the amplitude of the early-binary GWB depends on σ not only through the mass function but also through the suppression factors S1 and S2, marginalizing over σ does not merely integrate over a nuisance parameter; it averages over a range of model predictions whose reliability is not established for the larger σ values. The paper should report how the upper limits change if σ is restricted to, say, σ ≤ 0.3 or σ ≤ 0.5, so the reader can see the sensitivity of the headline f_PBH bounds to the unvalidated regime.
minor comments (4)
  1. [Sec. II] The sentence 'We concentrate on relatively narrow mass distributions (σ<1)' is misleading, because σ = 1 is not narrow: the log-normal mass function then spans a factor of e^4 ≈ 55 around µ. Please rephrase and make the prior choice in Table I consistent with the stated focus.
  2. [Sec. III, Eq. (7)] The calibration uncertainty parameter λ is introduced in Eq. (7) but its prior is not specified in the main text; please state the prior used (e.g., the Gaussian calibration-error model from the cited pygwb studies) or refer the reader to the relevant appendix or documentation.
  3. [Table II] The two-significant-figure entries in Table II give a false impression of precision given the model uncertainty documented in Appendix A; consider quoting one significant figure or adding a note about model dependence.
  4. [Conclusion] The claim that the paper presents 'for the first time, a direct GWB search specifically targeting PBH mergers' is overstated, since Refs. [25,27,51,55] already interpreted LVK stochastic data in terms of PBH merger backgrounds, and Ref. [55] used a full spectral model rather than a power-law approximation. I suggest softening the novelty claim to emphasize that this is the first combination of early and late formation channels with a full spectral shape.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the PBH-GWB limits come from a standard Bayesian fit of externally derived merger-rate models to public LVK cross-correlation data.

full rationale

The derivation chain is not circular. The likelihood (Eq. 7) compares the model spectrum Omega_GW = Omega_CBC + Omega_EB + Omega_LB to public LVK O1-O3 cross-correlation estimators [56-58], with detector noise variances entering via Eq. (17); the fitted parameters (mu, sigma, f_PBH, Omega_CBC) are inferred from the data, and the reported f_PBH values are posterior upper limits, not predictions derived from the same data by construction. The early- and late-binary merger rates (Eqs. 5-6) and the suppression factors S1, S2 (Eqs. 9-14) are adopted from external prior work [20,23,26,27,70-73], and R_clust is fixed to three reference values (1, 4e2, 1e3) rather than fitted; Table II shows the limits depend only weakly on R_clust, so the self-cited R_clust = 4e2 benchmark [30] is not load-bearing. The method is benchmarked against public LVK constraints and external PBH bounds rather than against the paper's own outputs. The Appendix A limitation that the suppression-factor expressions for broad mass distributions 'necessitates detailed analytical investigation or validation through N-body simulations' and that 'making claims based on these merging rates may be premature' is an important modeling-validity caveat, especially because sigma is marginalized up to 1 with a flat posterior, but it concerns the external rate model's domain of validity, not a reduction of the quoted limits to the paper's own inputs. No circular step can be exhibited.

Assumptions & free parameters 5 free parameters · 7 assumptions · 0 invented entities

The central claim rests on standard stochastic-background formalism plus several PBH population-model assumptions borrowed from the literature. The main contributors are the log-normal mass-function parametrization, the early-binary merger rate with suppression factors, the late-binary rate with a hand-chosen boost factor R_clust, and the power-law astrophysical CBC template. No new entities or ad hoc constants are introduced to force the result; the numbers that move the central claim are the fitted parameters mu, sigma, f_PBH, Omega_CBC, and the externally set R_clust.

free parameters (5)
  • mu (log-normal mean mass) = posterior; upper limits quoted at 1, 30, 1000 M_sun
    Fitted to data through nested sampling; prior log-uniform over [0.1, 1000] M_sun.
  • sigma (log-normal width) = weakly constrained; posterior roughly flat
    Fitted; prior log-uniform [0.01, 100]; injection study shows sigma is poorly recovered.
  • f_PBH = 95% C.L. upper limits: 3.3e-2 to 1.0 depending on mass and Rclust
    Fitted parameter; central result of the paper.
  • Omega_CBC = 95% upper limit ~3e-9
    Fitted amplitude of the astrophysical CBC power-law background; prior log-uniform [1e-10, 1e-7].
  • R_clust = 1, 4e2, 1e3 (three reference values)
    Not sampled; fixed to values from prior literature, including a value 4e2 motivated by GW event interpretations. The late-binary constraints depend on this choice.
assumptions (7)
  • standard math The Phinney relation (Eq. 4) correctly sums the gravitational-wave energy from all merging binaries into an isotropic background.
    Used to compute Omega_GW from merger rates; standard result [67].
  • domain assumption PBH mass function is log-normal and narrow (sigma < 1).
    Adopted in Sec. II; excludes broad mass functions such as QCD-inspired ones because their merger-rate modeling is uncertain.
  • domain assumption Early binary merger rate Eq. (5) and suppression factors S1, S2 in Appendix A are accurate enough for translating a GWB limit into f_PBH.
    Taken from Refs [20,26,27]; Appendix A warns that the expressions may be premature for broad mass distributions and that environment effects are incompletely understood.
  • domain assumption Late binary merger rate Eq. (6) with a single boost factor R_clust captures dynamical capture in PBH clusters.
    Based on [72-75]; R_clust is highly model-dependent (values from O(1) to O(10^3)).
  • domain assumption The unresolved astrophysical CBC background is a power law Omega_CBC (f/25 Hz)^(2/3).
    Standard approximation used in LVK stochastic searches; deviations are expected only above the sensitive band.
  • standard math The cross-correlation likelihood Eq. (7) is Gaussian and the calibration uncertainty parameter lambda is correctly marginalized.
    Standard radiometer formalism following [76,81,110,111].
  • domain assumption The public O1-O3 cross-correlation data and applied quality cuts are correctly propagated.
    The authors apply LVK vetoes following [56-58] but do not reproduce the full data-conditioning pipeline.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Search for a gravitational wave background from primordial black hole binaries using data from the first three LIGO-Virgo-KAGRA observing runs." pith.science (2026). https://pith.science/paper/HL5T6HXJ

@misc{pith2026241218318,
  author       = {Pith},
  title        = {Pith review of: Search for a gravitational wave background from primordial black hole binaries using data from the first three LIGO-Virgo-KAGRA observing runs},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HL5T6HXJ}},
  note         = {Machine review of arXiv:2412.18318}
}
read the original abstract

Using the cross-correlation data from the first three observing runs of the LIGO-Virgo-KAGRA Collaboration, we search for a gravitational-wave background (GWB) from primordial black holes, arising from the superposition of compact binary coalescence events. We consider both early and late binary formation mechanisms and perform Bayesian parameter inference. From the non-detection of the GWB, we provide constraints on the fraction of primordial black holes contributing to the present dark matter energy density.

Figures

Figures reproduced from arXiv: 2412.18318 by the authors.

Figure 1
Figure 1. FIG. 1. (Left) 95% C.L. constraints on [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. Binary suppression factors for early binary formation [PITH_FULL_IMAGE:figures/full_fig_p010_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. (Left) Posterior distributions from the injection study [PITH_FULL_IMAGE:figures/full_fig_p011_3.png] view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: FIG. 4. Corner plots of posteriors for [PITH_FULL_IMAGE:figures/full_fig_p012_4.png]
Figure 5
Figure 5. Figure 5: FIG. 5. Corner plots of posteriors for [PITH_FULL_IMAGE:figures/full_fig_p013_5.png]
Figure 6
Figure 6. Figure 6: FIG. 6. Corner plots of posteriors for [PITH_FULL_IMAGE:figures/full_fig_p014_6.png]

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Constraints on primordial black holes from the first part of LIGO-Virgo-KAGRA fourth observing run

    astro-ph.CO 2026-05 unverdicted novelty 6.0 of 10

    O4a gravitational-wave data give 95% CL upper limits f_PBH ~ 1e-2 to 1e-4 for monochromatic primordial black holes with mean masses 0.6-100 M_sun, with no evidence of a PBH merger component.

  2. Whispers from the Early Universe: The Ringdown of Primordial Black Holes

    astro-ph.CO 2025-07 conditional novelty 4.0 of 10

    The stochastic gravitational wave background from primordial black hole ringdown could be observable by future pulsar timing arrays for solar-mass and heavier black holes, with binary merger signals within reach of ne...

Reference graph

Works this paper leans on

112 extracted references · 75 canonical work pages · cited by 2 Pith papers

  1. [1]

    B. P. Abbott et al. Observation of Gravitational Waves from a Binary Black Hole Merger. Phys. Rev. Lett. , 116(6):061102, 2016

    2016

  2. [2]

    B. P. Abbott et al. GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observ- ing Runs. Phys. Rev. X , 9(3):031040, 2019

    2019

  3. [3]

    Gwtc-2: compact binary coales- cences observed by ligo and virgo during the first half of the third observing run

    Richard Abbott, TD Abbott, S Abraham, F Acernese, K Ackley, A Adams, C Adams, RX Adhikari, VB Adya, Christoph Affeldt, et al. Gwtc-2: compact binary coales- cences observed by ligo and virgo during the first half of the third observing run. Physical Review X, 11(2):021053, 2021

    2021

  4. [4]

    Abbott et al

    R. Abbott et al. GWTC-3: Compact Binary Coales- cences Observed by LIGO and Virgo during the Sec- ond Part of the Third Observing Run. Phys. Rev. X , 13(4):041039, 2023

    2023

  5. [5]

    Abbott et al

    R. Abbott et al. Tests of general relativity with binary black holes from the second LIGO-Virgo gravitational- wave transient catalog. Phys. Rev. D , 103(12):122002, 2021

    2021

  6. [6]

    Abbott et al

    R. Abbott et al. Constraints on the Cosmic Expansion History from GWTC–3. Astrophys. J., 949(2):76, 2023

    2023

  7. [7]

    The astrophysical gravitational wave stochastic background

    Tania Regimbau. The astrophysical gravitational wave stochastic background. Res. Astron. Astrophys., 11:369– 390, 2011

    2011

  8. [8]

    Turner, and Richard Watkins

    Arthur Kosowsky, Michael S. Turner, and Richard Watkins. Gravitational radiation from colliding vacuum bubbles. Phys. Rev. D , 45:4514–4535, 1992

    1992

Show all 112 references
  1. [9]

    Cal- lister, Huai-Ke Guo, Mario Mart ´ ınez, Mairi Sakellari- adou, Feng-Wei Yang, and Yue Zhao

    Alba Romero, Katarina Martinovic, Thomas A. Cal- lister, Huai-Ke Guo, Mario Mart ´ ınez, Mairi Sakellari- adou, Feng-Wei Yang, and Yue Zhao. Implications for First-Order Cosmological Phase Transitions from the Third LIGO-Virgo Observing Run. Phys. Rev. Lett. , 126(15):151301, 2021

    2021

  2. [10]

    Gravita- tional wave bursts from cosmic strings

    Thibault Damour and Alexander Vilenkin. Gravita- tional wave bursts from cosmic strings. Phys. Rev. Lett. , 85:3761–3764, 2000

    2000

  3. [11]

    Abbott et al

    R. Abbott et al. Constraints on Cosmic Strings Using Data from the Third Advanced LIGO–Virgo Observing Run. Phys. Rev. Lett. , 126(24):241102, 2021

    2021

  4. [12]

    Starobinsky

    Alexei A. Starobinsky. Spectrum of relict gravitational radiation and the early state of the universe. JETP Lett., 30:682–685, 1979

    1979

  5. [13]

    Figueroa

    Chiara Caprini and Daniel G. Figueroa. Cosmological Backgrounds of Gravitational Waves. Class. Quant. Grav., 35(16):163001, 2018

    2018

  6. [14]

    Gravitational Waves: The Theo- rist’s Swiss Knife

    Mairi Sakellariadou. Gravitational Waves: The Theo- rist’s Swiss Knife. Universe, 8(2):132, 2022

    2022

  7. [15]

    Gravitationally collapsed objects of very low mass

    Stephen Hawking. Gravitationally collapsed objects of very low mass. Monthly Notices of the Royal Astronomi- cal Society, 152(1):75–78, 1971

    1971

  8. [16]

    Cosmological effects of primordial black holes

    George F Chapline. Cosmological effects of primordial black holes. Nature, 253(5489):251–252, 1975

    1975

  9. [17]

    Primordial black holes as dark matter candidates

    Bernard Carr and Florian Kuhnel. Primordial black holes as dark matter candidates. SciPost Phys. Lect. Notes, 48:1, 2022

    2022

  10. [18]

    Primordial black holes as a dark matter candidate

    Anne M Green and Bradley J Kavanagh. Primordial black holes as a dark matter candidate. Journal of Physics G: Nuclear and Particle Physics , 48(4):043001, 2021

    2021

  11. [19]

    Mu˜ noz, Yacine Ali- Ha ¨ ımoud, Marc Kamionkowski, Ely D

    Simeon Bird, Ilias Cholis, Julian B. Mu˜ noz, Yacine Ali- Ha ¨ ımoud, Marc Kamionkowski, Ely D. Kovetz, Alvise Raccanelli, and Adam G. Riess. Did LIGO detect dark matter? Phys. Rev. Lett. , 116(20):201301, 2016

    2016

  12. [20]

    Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914

    Misao Sasaki, Teruaki Suyama, Takahiro Tanaka, and Shuichiro Yokoyama. Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. Phys. Rev. Lett., 117(6):061101, 2016. [Erratum: Phys.Rev.Lett. 121, 059901 (2018)]

    2018

  13. [21]

    The cluster- ing of massive Primordial Black Holes as Dark Matter: measuring their mass distribution with Advanced LIGO

    Sebastien Clesse and Juan Garc ´ ıa-Bellido. The cluster- ing of massive Primordial Black Holes as Dark Matter: measuring their mass distribution with Advanced LIGO. Phys. Dark Univ. , 15:142–147, 2017

    2017

  14. [22]

    Properties and astrophysical implica- tions of the 150 m⊙ binary black hole merger gw190521

    Richard Abbott, TD Abbott, S Abraham, F Acernese, K Ackley, C Adams, RX Adhikari, VB Adya, C Affeldt, M Agathos, et al. Properties and astrophysical implica- tions of the 150 m⊙ binary black hole merger gw190521. The Astrophysical Journal Letters , 900(1):L13, 2020

    2020

  15. [23]

    Merger rate of primordial black-hole binaries

    Yacine Ali-Ha ¨ ımoud, Ely D Kovetz, and Marc Kamionkowski. Merger rate of primordial black-hole binaries. Physical Review D , 96(12):123523, 2017

    2017

  16. [24]

    Seven hints for primordial black hole dark matter

    Sebastien Clesse and Juan Garc ´ ıa-Bellido. Seven hints for primordial black hole dark matter. Physics of the Dark Universe , 22:137–146, 2018

    2018

  17. [25]

    Grav- itational Waves from Primordial Black Hole Mergers

    Martti Raidal, Ville Vaskonen, and Hardi Veerm¨ ae. Grav- itational Waves from Primordial Black Hole Mergers. JCAP, 09:037, 2017

    2017

  18. [26]

    Formation and Evolution of Primor- dial Black Hole Binaries in the Early Universe

    Martti Raidal, Christian Spethmann, Ville Vaskonen, and Hardi Veerm¨ ae. Formation and Evolution of Primor- dial Black Hole Binaries in the Early Universe. JCAP, 02:018, 2019. 7

    2019

  19. [27]

    Two populations of LIGO-Virgo black holes

    Gert H¨ utsi, Martti Raidal, Ville Vaskonen, and Hardi Veerm¨ ae. Two populations of LIGO-Virgo black holes. JCAP, 03:068, 2021

    2021

  20. [28]

    Lower bound on the primordial black hole merger rate

    Ville Vaskonen and Hardi Veerm¨ ae. Lower bound on the primordial black hole merger rate. Phys. Rev. D , 101(4):043015, 2020

    2020

  21. [29]

    Pul- sar Timing Array Constraints on Primordial Black Holes with NANOGrav 11-Year Dataset

    Zu-Cheng Chen, Chen Yuan, and Qing-Guo Huang. Pul- sar Timing Array Constraints on Primordial Black Holes with NANOGrav 11-Year Dataset. Phys. Rev. Lett. , 124(25):251101, 2020

    2020

  22. [30]

    Gw190425, gw190521 and gw190814: Three candidate mergers of primordial black holes from the qcd epoch

    Sebastien Clesse and Juan Garcia-Bellido. Gw190425, gw190521 and gw190814: Three candidate mergers of primordial black holes from the qcd epoch. Physics of the Dark Universe , 38:101111, 2022

    2022

  23. [31]

    Gw190521 mass gap event and the pri- mordial black hole scenario

    V De Luca, V Desjacques, G Franciolini, P Pani, and A Riotto. Gw190521 mass gap event and the pri- mordial black hole scenario. Physical review letters , 126(5):051101, 2021

    2021

  24. [32]

    Primordial black holes and uncertainties in the choice of the window function

    Kenta Ando, Keisuke Inomata, and Masahiro Kawasaki. Primordial black holes and uncertainties in the choice of the window function. Physical Review D , 97(10):103528, 2018

    2018

  25. [33]

    Blinnikov, A

    S. Blinnikov, A. Dolgov, N. K. Porayko, and K. Postnov. Solving puzzles of GW150914 by primordial black holes. JCAP, 11:036, 2016

    2016

  26. [34]

    Gow, and Christian T

    Alex Hall, Andrew D. Gow, and Christian T. Byrnes. Bayesian analysis of LIGO-Virgo mergers: Primordial vs. astrophysical black hole populations. Phys. Rev. D , 102:123524, 2020

    2020

  27. [35]

    Kaze W. K. Wong, Gabriele Franciolini, Valerio De Luca, Vishal Baibhav, Emanuele Berti, Paolo Pani, and An- tonio Riotto. Constraining the primordial black hole scenario with Bayesian inference and machine learning: the GWTC-2 gravitational wave catalog. Phys. Rev. D , 103(2):...

    2021

  28. [36]

    Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates

    Karsten Jedamzik. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett., 126(5):051302, 2021

    2021

  29. [37]

    De Luca, G

    V. De Luca, G. Franciolini, P. Pani, and A. Riotto. Bayesian Evidence for Both Astrophysical and Primor- dial Black Holes: Mapping the GWTC-2 Catalog to Third-Generation Detectors. JCAP, 05:003, 2021

    2021

  30. [38]

    Hierarchical Black-Hole Merg- ers in Multiple Systems: Constrain the Formation of GW190412, GW190814 and GW190521-like events

    Bin Liu and Dong Lai. Hierarchical Black-Hole Merg- ers in Multiple Systems: Constrain the Formation of GW190412, GW190814 and GW190521-like events. Mon. Not. Roy. Astron. Soc. , 502(2):2049–2064, 2021

    2021

  31. [39]

    Goldstein, and Savvas M

    Kyriakos Vattis, Isabelle S. Goldstein, and Savvas M. Koushiappas. Could the 2.6 M⊙ object in GW190814 be a primordial black hole? Phys. Rev. D , 102(6):061301, 2020

    2020

  32. [40]

    De Luca, G

    V. De Luca, G. Franciolini, P. Pani, and A. Riotto. Pri- mordial Black Holes Confront LIGO/Virgo data: Cur- rent situation. JCAP, 06:044, 2020

    2020

  33. [41]

    Confronting Primordial Black Holes with LIGO-Virgo-KAGRA and the Einstein Telescope, page 617–650

    Zu-Cheng Chen and Alex Hall. Confronting Primordial Black Holes with LIGO-Virgo-KAGRA and the Einstein Telescope, page 617–650. Springer Nature Singapore, 2025

    2025

  34. [42]

    Can we distin- guish astrophysical from primordial black holes via the stochastic gravitational wave background? Mon

    Suvodip Mukherjee and Joseph Silk. Can we distin- guish astrophysical from primordial black holes via the stochastic gravitational wave background? Mon. Not. Roy. Astron. Soc., 506(3):3977–3985, 2021

    2021

  35. [43]

    Gw190521: a bi- nary black hole merger with a total mass of 150 m⊙

    Richard Abbott, TD Abbott, S Abraham, Fausto Ac- ernese, K Ackley, C Adams, RX Adhikari, VB Adya, Christoph Affeldt, M Agathos, et al. Gw190521: a bi- nary black hole merger with a total mass of 150 m⊙. Physical review letters , 125(10):101102, 2020

    2020

  36. [44]

    Gabriele Franciolini, Vishal Baibhav, Valerio De Luca, Ken K. Y. Ng, Kaze W. K. Wong, Emanuele Berti, Paolo Pani, Antonio Riotto, and Salvatore Vitale. Searching for a subpopulation of primordial black holes in LIGO-Virgo gravitational-wave data. Phys. Rev. D , 105(8):083526, 2022

    2022

  37. [45]

    Broad search for gravitational waves from subsolar-mass binaries through ligo and virgo’s third observing run

    Alexander H Nitz and Yi-Fan Wang. Broad search for gravitational waves from subsolar-mass binaries through ligo and virgo’s third observing run. Physical Review D , 106(2):023024, 2022

    2022

  38. [46]

    Kapadia, Ryan Magee, and An- dres Jorge Tanasijczuk

    Khun Sang Phukon, Gregory Baltus, Sarah Caudill, Se- bastien Clesse, Antoine Depasse, Maxime Fays, Heather Fong, Shasvath J. Kapadia, Ryan Magee, and An- dres Jorge Tanasijczuk. The hunt for sub-solar pri- mordial black holes in low mass ratio binaries is open. arXiv:2105.11449

    arXiv

  39. [47]

    Abbott et al

    R. Abbott et al. Search for subsolar-mass black hole binaries in the second part of Advanced LIGO’s and Advanced Virgo’s third observing run. Mon. Not. Roy. Astron. Soc. , 524(4):5984–5992, 2023. [Erratum: Mon.Not.Roy.Astron.Soc. 526, 6234 (2023)]

    2023

  40. [48]

    Miller, Nancy Aggarwal, S´ ebastien Clesse, Federico De Lillo, Surabhi Sachdev, Pia Astone, Cris- tiano Palomba, Ornella J

    Andrew L. Miller, Nancy Aggarwal, S´ ebastien Clesse, Federico De Lillo, Surabhi Sachdev, Pia Astone, Cris- tiano Palomba, Ornella J. Piccinni, and Lorenzo Pierini. Gravitational Wave Constraints on Planetary-Mass Pri- mordial Black Holes Using LIGO O3a Data. Phys. Rev. Lett.,...

    2024

  41. [49]

    C´ eline Boehm, Archil Kobakhidze, Ciaran A. J. O’hare, Zachary S. C. Picker, and Mairi Sakellariadou. Elimi- nating the LIGO bounds on primordial black hole dark matter. JCAP, 03:078, 2021

    2021

  42. [50]

    Stochas- tic gravitational-wave background due to primordial binary black hole mergers

    Vuk Mandic, Simeon Bird, and Ilias Cholis. Stochas- tic gravitational-wave background due to primordial binary black hole mergers. Physical review letters , 117(20):201102, 2016

    2016

  43. [51]

    Constraints on the primordial black hole abun- dance from the first advanced ligo observation run using the stochastic gravitational-wave background

    Sai Wang, Yi-Fan Wang, Qing-Guo Huang, and Tjon- nie GF Li. Constraints on the primordial black hole abun- dance from the first advanced ligo observation run using the stochastic gravitational-wave background. Physical Review Letters, 120(19):191102, 2018

    2018

  44. [52]

    Detected stochastic gravitational waves and subsolar-mass primordial black holes

    Keisuke Inomata, Kazunori Kohri, and Takahiro Ter- ada. Detected stochastic gravitational waves and subsolar-mass primordial black holes. Phys. Rev. D , 109(6):063506, 2024

    2024

  45. [53]

    Suvodip Mukherjee, Matthew S. P. Meinema, and Joseph Silk. Prospects of discovering subsolar primordial black holes using the stochastic gravitational wave background from third-generation detectors. Mon. Not. Roy. Astron. Soc., 510(4):6218–6224, 2022

    2022

  46. [54]

    LIGO-Virgo-KAGRA Constraints on Primordial Black Holes from Stochastic Gravitational-Wave Background Searches, pages 651–688

    Alba Romero-Rodr ´ ıguez and Sachiko Kuroyanagi. LIGO-Virgo-KAGRA Constraints on Primordial Black Holes from Stochastic Gravitational-Wave Background Searches, pages 651–688. Springer Nature Singapore, Singapore, 2025

    2025

  47. [55]

    Blanco-Pillado, Albert Sanglas, and Nikolaos Triantafyllou

    Vicente Atal, Jose J. Blanco-Pillado, Albert Sanglas, and Nikolaos Triantafyllou. Constraining changes in the merger history of BH and PBH binaries with the stochastic gravitational wave background. Phys. Rev. D , 105(12):123522, 2022

    2022

  48. [56]

    Upper limits on the stochastic gravitational-wave background from advanced ligo’s first observing run

    Benjamin P Abbott, Robert Abbott, Thomas D Ab- bott, Matthew R Abernathy, Fausto Acernese, Kendall 8 Ackley, Carl Adams, Thomas Adams, Paolo Addesso, Rana X Adhikari, et al. Upper limits on the stochastic gravitational-wave background from advanced ligo’s first observing run. ...

    2017

  49. [57]

    Search for the isotropic stochastic back- ground using data from advanced ligo’s second observing run

    Benjamin P Abbott, R Abbott, TD Abbott, S Abraham, F Acernese, K Ackley, C Adams, VB Adya, C Affeldt, M Agathos, et al. Search for the isotropic stochastic back- ground using data from advanced ligo’s second observing run. Physical Review D , 100(6):061101, 2019

    2019

  50. [58]

    Upper limits on the isotropic gravitational-wave background from advanced ligo and advanced virgo’s third observing run

    Ryan Abbott, TD Abbott, S Abraham, Fausto Acer- nese, K Ackley, A Adams, C Adams, Rana X Adhikari, VB Adya, C Affeldt, et al. Upper limits on the isotropic gravitational-wave background from advanced ligo and advanced virgo’s third observing run. Physical Review D, 104(2):022004, 2021

    2021

  51. [59]

    Primordial black hole formation during the QCD epoch

    Karsten Jedamzik. Primordial black hole formation during the QCD epoch. Phys. Rev. D , 55:5871–5875, 1997

    1997

  52. [60]

    Cosmic conundra explained by thermal history and primordial black holes

    Bernard Carr, Sebastien Clesse, Juan Garc ´ ıa-Bellido, and Florian K¨ uhnel. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Univ., 31:100755, 2021

    2021

  53. [61]

    Primordial black holes from the QCD epoch: Linking dark matter, baryogenesis and anthropic selection

    Bernard Carr, Sebastien Clesse, and Juan Garc ´ ıa-Bellido. Primordial black holes from the QCD epoch: Linking dark matter, baryogenesis and anthropic selection. Mon. Not. Roy. Astron. Soc. , 501(1):1426–1439, 2021

    2021

  54. [62]

    Gow, Christian T

    Andrew D. Gow, Christian T. Byrnes, and Alex Hall. Accurate model for the primordial black hole mass dis- tribution from a peak in the power spectrum. Phys. Rev. D, 105(2):023503, 2022

    2022

  55. [63]

    Baryon isocurvature fluctuations at small scales and baryonic dark matter

    Alexandre Dolgov and Joseph Silk. Baryon isocurvature fluctuations at small scales and baryonic dark matter. Phys. Rev. D , 47:4244–4255, May 1993

    1993

  56. [64]

    De Luca, G

    V. De Luca, G. Franciolini, and A. Riotto. On the primordial black hole mass function for broad spectra. Phys. Lett. B , 807:135550, 2020

    2020

  57. [65]

    Primordial non- Gaussianity up to all orders: Theoretical aspects and implications for primordial black hole models

    Giacomo Ferrante, Gabriele Franciolini, Antonio Iovino, Junior., and Alfredo Urbano. Primordial non- Gaussianity up to all orders: Theoretical aspects and implications for primordial black hole models. Phys. Rev. D, 107(4):043520, 2023

    2023

  58. [66]

    Gow, Hooshyar Assadullahi, Joseph H

    Andrew D. Gow, Hooshyar Assadullahi, Joseph H. P. Jackson, Kazuya Koyama, Vincent Vennin, and David Wands. Non-perturbative non-Gaussianity and primor- dial black holes. EPL, 142(4):49001, 2023

    2023

  59. [67]

    E. S. Phinney. A Practical theorem on gravitational wave backgrounds. 7 2001

    2001

  60. [68]

    Inspiral- merger-ringdown waveforms for black-hole binaries with nonprecessing spins

    P Ajith, Mark Hannam, Sascha Husa, Yanbei Chen, B Br¨ ugmann, Nils Dorband, D M¨ uller, Frank Ohme, Denis Pollney, Christian Reisswig, et al. Inspiral- merger-ringdown waveforms for black-hole binaries with nonprecessing spins. Physical Review Letters , 106(24):241101, 2011

    2011

  61. [69]

    Takashi Nakamura, Misao Sasaki, Takahiro Tanaka, and Kip S. Thorne. Gravitational waves from coalescing black hole MACHO binaries. Astrophys. J. Lett. , 487:L139– L142, 1997

    1997

  62. [70]

    Black hole binary formation in the expanding universe: Three body problem approximation

    Kunihito Ioka, Takeshi Chiba, Takahiro Tanaka, and Takashi Nakamura. Black hole binary formation in the expanding universe: Three body problem approximation. Physical Review D , 58(6):063003, 1998

    1998

  63. [71]

    Hidden universality in the merger rate distribution in the primordial black hole scenario

    Bence Kocsis, Teruaki Suyama, Takahiro Tanaka, and Shuichiro Yokoyama. Hidden universality in the merger rate distribution in the primordial black hole scenario. The Astrophysical Journal , 854(1):41, 2018

    2018

  64. [72]

    Quinlan and Stuart L

    Gerald D. Quinlan and Stuart L. Shapiro. Dynamical Evolution of Dense Clusters of Compact Stars.Astrophys. J., 343:725, August 1989

    1989

  65. [73]

    Runaway merg- ing of black holes: analytical constraint on the timescale

    Hideaki Mouri and Yoshiaki Taniguchi. Runaway merg- ing of black holes: analytical constraint on the timescale. Astrophys. J. Lett. , 566:L17–L20, 2002

    2002

  66. [74]

    Mu˜ noz, Yacine Ali- Ha ¨ ımoud, Marc Kamionkowski, Ely D

    Simeon Bird, Ilias Cholis, Julian B. Mu˜ noz, Yacine Ali- Ha ¨ ımoud, Marc Kamionkowski, Ely D. Kovetz, Alvise Raccanelli, and Adam G. Riess. Did ligo detect dark matter? Phys. Rev. Lett. , 116:201301, May 2016

    2016

  67. [75]

    A boosted gravita- tional wave background for primordial black holes with broad mass distributions and thermal features

    Eleni Bagui and Sebastien Clesse. A boosted gravita- tional wave background for primordial black holes with broad mass distributions and thermal features. Physics of the Dark Universe , 38:101115, 2022

    2022

  68. [76]

    and closely follows that of previous studies [57, 58, 77– 85], with specific adaptations to our analysis. We utilize data from the Advanced LIGO detectors located in Hanford (H) and Livingston (L), as well as data from the Virgo (V) observatory, during the first three observin...

    2023

  69. [77]

    Parameter estimation in searches for the stochastic gravitational-wave background

    Vuk Mandic, Eric Thrane, Stefanos Giampanis, and Tania Regimbau. Parameter estimation in searches for the stochastic gravitational-wave background. Physical review letters, 109(17):171102, 2012

    2012

  70. [78]

    Searching for parity violation with the ligo-virgo-kagra network

    Katarina Martinovic, Charles Badger, Mairi Sakellari- adou, and Vuk Mandic. Searching for parity violation with the ligo-virgo-kagra network. Physical Review D , 104(8):L081101, 2021

    2021

  71. [79]

    Search for a scalar induced stochastic gravitational wave background in the third ligo-virgo observing run

    Alba Romero-Rodriguez, Mario Martinez, Oriol Pujolas, Mairi Sakellariadou, and Ville Vaskonen. Search for a scalar induced stochastic gravitational wave background in the third ligo-virgo observing run. Physical review letters, 128(5):051301, 2022

    2022

  72. [80]

    Probing early universe supercooled phase transitions with gravitational wave data

    Charles Badger, Bartosz Fornal, Katarina Martinovic, Alba Romero, Kevin Turbang, Huai-Ke Guo, Alberto Mariotti, Mairi Sakellariadou, Alexander Sevrin, Feng- Wei Yang, et al. Probing early universe supercooled phase transitions with gravitational wave data. Physical Review D, 1...

    2023

  73. [81]

    Detection prospects of gravitational waves from su (2) axion inflation

    Charles Badger, Hannah Duval, Tomohiro Fujita, Sachiko Kuroyanagi, Alba Romero-Rodr ´ ıguez, and Mairi Sakellariadou. Detection prospects of gravitational waves from su (2) axion inflation. Physical Review D , 110(8):084063, 2024

    2024

  74. [82]

    pygwb: A python-based library for gravitational-wave background searches

    Arianna I Renzini, Alba Romero-Rodr ´ ıguez, Colm Tal- bot, Max Lalleman, Shivaraj Kandhasamy, Kevin Tur- bang, Sylvia Biscoveanu, Katarina Martinovic, Patrick Meyers, Leo Tsukada, et al. pygwb: A python-based library for gravitational-wave background searches. The Astrophysic...

    2023

  75. [83]

    Accessibility of the stochastic gravitational wave back- ground from magnetars to the interferometric gravita- tional wave detectors

    Cheng-Jian Wu, Vuk Mandic, and Tania Regimbau. Accessibility of the stochastic gravitational wave back- ground from magnetars to the interferometric gravita- tional wave detectors. Physical Review D—Particles, Fields, Gravitation, and Cosmology , 87(4):042002, 2013

    2013

  76. [84]

    Measurement of parity violation in the early universe using gravitational-wave detectors

    SG Crowder, R Namba, V Mandic, S Mukohyama, and M Peloso. Measurement of parity violation in the early universe using gravitational-wave detectors. Physics Letters B, 726(1-3):66–71, 2013

    2013

  77. [85]

    Model of the stochastic gravitational-wave background due to core collapse to black holes

    Kyle Crocker, V Mandic, T Regimbau, K Belczynski, W Gladysz, K Olive, T Prestegard, and E Vangioni. Model of the stochastic gravitational-wave background due to core collapse to black holes. Physical Review D , 92(6):063005, 2015

    2015

  78. [86]

    Multiwavelength ob- servations of cosmological phase transitions using lisa and cosmic explorer

    Margot Fitz Axen, Sharan Banagiri, Andrew Matas, Chiara Caprini, and Vuk Mandic. Multiwavelength ob- servations of cosmological phase transitions using lisa and cosmic explorer. Physical Review D , 98(10):103508, 9 2018

    2018

  79. [87]

    Increasing the astrophysical reach of the advanced virgo detector via the application of squeezed vacuum states of light

    Fausto Acernese, M Agathos, L Aiello, A Allocca, A Am- ato, S Ansoldi, S Antier, M Ar` ene, N Arnaud, S Ascenzi, et al. Increasing the astrophysical reach of the advanced virgo detector via the application of squeezed vacuum states of light. Physical review letters , 123(23):2...

    2019

  80. [88]

    Gw150914: The advanced ligo detectors in the era of first discoveries

    Benjamin P Abbott, R Abbott, TD Abbott, MR Aber- nathy, Fausto Acernese, K Ackley, C Adams, T Adams, Paolo Addesso, RX Adhikari, et al. Gw150914: The advanced ligo detectors in the era of first discoveries. Physical review letters , 116(13):131103, 2016

    2016

  81. [89]

    Sensitivity and performance of the advanced ligo detectors in the third observing run

    Aaron Buikema, Craig Cahillane, GL Mansell, CD Blair, Robert Abbott, C Adams, RX Adhikari, A Ananyeva, S Appert, K Arai, et al. Sensitivity and performance of the advanced ligo detectors in the third observing run. Physical Review D , 102(6):062003, 2020

    2020

  82. [90]

    Abbott et al

    R. Abbott et al. Open Data from the Third Observing Run of LIGO, Virgo, KAGRA, and GEO. Astrophys. J. Suppl., 267(2):29, 2023

    2023

  83. [91]

    Treatment of calibration uncertainty in multi-baseline cross-correlation searches for gravita- tional waves

    John T Whelan, Emma L Robinson, Joseph D Romano, and Eric H Thrane. Treatment of calibration uncertainty in multi-baseline cross-correlation searches for gravita- tional waves. In Journal of Physics: Conference Series , volume 484, page 012027. IOP Publishing, 2014

    2014

  84. [92]

    Characterization of systematic error in ad- vanced ligo calibration

    Ling Sun, Evan Goetz, Jeffrey S Kissel, Joseph Bet- zwieser, Sudarshan Karki, Aaron Viets, Madeline Wade, Dripta Bhattacharjee, Vladimir Bossilkov, Pep B Co- vas, et al. Characterization of systematic error in ad- vanced ligo calibration. Classical and Quantum Gravity , 37(22)...

    2020

  85. [93]

    Limits on stellar-mass compact objects as dark matter from gravi- tational lensing of type ia supernovae

    Miguel Zumalacarregui and Uroˇ s Seljak. Limits on stellar-mass compact objects as dark matter from gravi- tational lensing of type ia supernovae. Physical review letters, 121(14):141101, 2018

    2018

  86. [94]

    Limits on the macho con- tent of the galactic halo from the eros-2 survey of the mag- ellanic clouds

    Patrick Tisserand, L Le Guillou, C Afonso, JN Al- bert, J Andersen, R Ansari, ´E Aubourg, P Bareyre, JP Beaulieu, X Charlot, et al. Limits on the macho con- tent of the galactic halo from the eros-2 survey of the mag- ellanic clouds. Astronomy & Astrophysics , 469(2):387– 404, 2007

    2007

  87. [95]

    No massive black holes in the milky way halo

    Przemek Mr´ oz, Andrzej Udalski, Micha l K Szyma´ nski, Igor Soszy´ nski, Lukasz Wyrzykowski, Pawe l Pietrukow- icz, Szymon Koz lowski, Rados law Poleski, Jan Skowron, Dorota Skowron, et al. No massive black holes in the milky way halo. Nature, 632(8026):749–751, 2024

    2024

  88. [96]

    Feedback in the dark: a critical examination of CMB bounds on primordial black holes

    Dominic Agius, Rouven Essig, Daniele Gaggero, Francesca Scarcella, Gregory Suczewski, and Mauro Valli. Feedback in the dark: a critical examination of CMB bounds on primordial black holes. JCAP, 07:003, 2024

    2024

  89. [97]

    Kavanagh

    Bradley J. Kavanagh. PBH bounds. https://github. com/bradkav/PBHbounds

  90. [98]

    Limits of astrophysics with gravitational-wave backgrounds

    Thomas Callister, Letizia Sammut, Shi Qiu, Ilya Man- del, and Eric Thrane. Limits of astrophysics with gravitational-wave backgrounds. Physical Review X , 6(3):031018, 2016

    2016

  91. [99]

    Bayes in the sky: Bayesian inference and model selection in cosmology

    Roberto Trotta. Bayes in the sky: Bayesian inference and model selection in cosmology. Contemp. Phys. , 49:71–104, 2008

    2008

  92. [100]

    Andr´ es-Carcasona, A

    M. Andr´ es-Carcasona, A. J. Iovino, V. Vaskonen, H. Veerm¨ ae, M. Mart ´ ınez, O. Pujol` as, and Ll. M. Mir. Constraints on primordial black holes from LIGO-Virgo- KAGRA O3 events. Phys. Rev. D , 110(2):023040, 2024

    2024

  93. [101]

    dynesty: a dynamic nested sam- pling package for estimating bayesian posteriors and evidences

    Joshua S Speagle. dynesty: a dynamic nested sam- pling package for estimating bayesian posteriors and evidences. Monthly Notices of the Royal Astronomical Society, 493(3):3132–3158, 2020

    2020

  94. [102]

    Monte carlo and quasi-monte carlo methods

    Russel E Caflisch. Monte carlo and quasi-monte carlo methods. Acta numerica, 7:1–49, 1998

    1998

  95. [103]

    Punturo et al

    M. Punturo et al. The Einstein Telescope: A third- generation gravitational wave observatory. Class. Quant. Grav., 27:194002, 2010

    2010

  96. [104]

    Sensitivity studies for third-generation gravitational wave observatories

    S Hild, M Abernathy, F ea Acernese, P Amaro-Seoane, N Andersson, K Arun, F Barone, B Barr, M Barsuglia, M Beker, et al. Sensitivity studies for third-generation gravitational wave observatories. Classical and Quantum gravity, 28(9):094013, 2011

    2011

  97. [105]

    Exploring the sensitivity of next generation gravitational wave detectors

    Benjamin P Abbott, Richard Abbott, Thomas D Abbott, Matthew R Abernathy, Kendall Ackley, Carl Adams, Paolo Addesso, Rana X Adhikari, Vaishali B Adya, Christoph Affeldt, et al. Exploring the sensitivity of next generation gravitational wave detectors. Classical and Quantum Grav...

    2017

  98. [106]

    Cosmic Explorer: The U.S

    David Reitze et al. Cosmic Explorer: The U.S. Contri- bution to Gravitational-Wave Astronomy beyond LIGO. Bull. Am. Astron. Soc. , 51(7):035, 2019

    2019

  99. [107]

    Matplotlib: A 2d graphics environment

    John D Hunter. Matplotlib: A 2d graphics environment. Computing in science & engineering , 9(03):90–95, 2007

    2007

  100. [108]

    The numpy array: a structure for efficient numer- ical computation

    Stefan Van Der Walt, S Chris Colbert, and Gael Varo- quaux. The numpy array: a structure for efficient numer- ical computation. Computing in science & engineering , 13(2):22–30, 2011

    2011

  101. [109]

    Scipy 1.0: fundamental algorithms for sci- entific computing in python

    Pauli Virtanen, Ralf Gommers, Travis E Oliphant, Matt Haberland, Tyler Reddy, David Cournapeau, Evgeni Burovski, Pearu Peterson, Warren Weckesser, Jonathan Bright, et al. Scipy 1.0: fundamental algorithms for sci- entific computing in python. Nature methods, 17(3):261– 272, 2020

    2020

  102. [110]

    Primordial black holes and their gravitational-wave signatures

    Eleni Bagui et al. Primordial black holes and their gravitational-wave signatures. Living Rev. Rel. , 28(1):1, 2025

    2025

  103. [111]

    Bruce Allen and Joseph D. Romano. Detecting a stochas- tic background of gravitational radiation: Signal process- ing strategies and sensitivities. Phys. Rev. D , 59:102001, 1999

    1999

  104. [112]

    Detection meth- ods for stochastic gravitational-wave backgrounds: a unified treatment

    Joseph D Romano and Neil J Cornish. Detection meth- ods for stochastic gravitational-wave backgrounds: a unified treatment. Living reviews in relativity , 20:1–223, 2017. 10 APPENDIX A: MODELS FOR SUPPRESSION F ACTORS Here we give for completeness the models for binary suppres...

    2017

Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.