arxiv: 2604.06082 · v1 · submitted 2026-04-07 · 🌌 astro-ph.CO · gr-qc

Recognition: 2 theorem links

· Lean Theorem

Hunting Dark Matter with the Einstein Telescope

A.J. Iovino , M. Maggiore , N. Muttoni , A. Riotto

Authors on Pith no claims yet

Pith reviewed 2026-05-10 18:09 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qc

keywords primordial black holesdark matterstochastic gravitational wavesEinstein Telescopeclustered formationhalo collapse

0 comments

The pith

Light primordial black holes formed in dense clusters can collapse into heavier ones that account for all dark matter while producing a detectable flat gravitational-wave background.

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

The paper shows that very light primordial black holes, normally ruled out because they evaporate and distort the cosmic microwave background, can avoid those bounds if they form in strong clusters. In this setup the clusters collapse into heavier black holes that could comprise the entire dark matter density. The process generates a flat spectrum of stochastic gravitational waves whose amplitude and frequency range fall within the sensitivity of the Einstein Telescope.

Core claim

If primordial black holes are formed strongly clustered, the corresponding haloes may collapse in heavier black holes which may form the entirety of the dark matter of the universe. The indirect signal of such scenario is the production of a flat stochastic background of gravitational waves which is detectable by the Einstein Telescope.

What carries the argument

Strong clustering of light primordial black holes that drives halo collapse into heavier black holes and sources a flat stochastic gravitational-wave background.

If this is right

Light primordial black holes can constitute all dark matter without violating evaporation or CMB constraints.
The gravitational-wave background is predicted to be flat and to lie in the frequency window accessible to the Einstein Telescope.
Detection of this background would constitute indirect evidence that dark matter consists of primordial black holes formed through clustered collapse.
The mechanism links early-universe clustering physics directly to a concrete observational signature.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

Confirmation would motivate searches for the specific initial clustering spectrum required by inflation or other early-universe models.
A measured amplitude could be cross-checked against microlensing or other primordial-black-hole bounds to tighten the allowed mass window.
Absence of the signal would push clustered formation scenarios toward lower efficiencies or different mass distributions.

Load-bearing premise

Primordial black holes must form in sufficiently dense clusters for their haloes to collapse into heavier black holes before evaporating.

What would settle it

A null result from the Einstein Telescope showing no flat stochastic gravitational-wave background in the relevant frequency band would rule out the clustered primordial black hole dark-matter scenario.

read the original abstract

Too light primordial black holes evaporate and are therefore strongly constrained by various bounds, e.g. Cosmic Microwave Background distortion. However, if they are formed strongly clustered, the corresponding haloes may collapse in heavier black holes which may form the entirety of the dark matter of the universe. The indirect signal of such scenario is the production of a flat stochastic background of gravitational waves which is detectable by the Einstein Telescope.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

The paper argues that strongly clustered light primordial black holes can collapse into heavier ones making up all dark matter and produce a flat stochastic gravitational wave background detectable by the Einstein Telescope, but the supporting calculations for the spectrum and amplitude are not shown in enough detail to verify.

read the letter

The core claim is that light PBHs, normally ruled out by evaporation bounds, could still comprise all dark matter if they form in tight clusters whose halos collapse into heavier black holes, and that this collapse process generates a flat SGWB reachable by ET. That is the one thing a colleague should take away first: it is an attempt to turn a clustering assumption into a concrete GW target for a future detector.

Referee Report

2 major / 0 minor

Summary. The manuscript argues that too-light primordial black holes (PBHs), normally ruled out by evaporation and CMB constraints, can evade these bounds if formed with strong clustering. The resulting haloes collapse into heavier black holes that could constitute all dark matter; the indirect observable is a flat stochastic gravitational-wave background (SGWB) detectable by the Einstein Telescope.

Significance. If the clustering-to-collapse mechanism and the resulting flat SGWB can be shown to arise from a concrete model with amplitude above ET sensitivity, the scenario would link light PBHs to the full DM density while predicting a distinctive, testable GW signal. This would be a notable addition to PBH-DM phenomenology, provided the quantitative steps are supplied.

major comments (2)

[Abstract] Abstract: the statement that 'the corresponding haloes may collapse in heavier black holes which may form the entirety of the dark matter' is presented without any derivation of the minimum clustering strength, overdensity threshold, or collapse timescale relative to the evaporation time. This assumption is load-bearing for the entire proposal.
[Abstract] Abstract: the claim that the scenario produces 'a flat stochastic background of gravitational waves which is detectable by the Einstein Telescope' is asserted without a spectrum calculation, strain amplitude estimate, frequency range, or comparison to the ET noise curve. No equation or figure supports the flatness or the detectability assertion.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading of our manuscript and the constructive comments. We agree that the current version, which is a concise proposal outlining a novel scenario, lacks the quantitative details requested. We will revise the manuscript to incorporate the necessary derivations, calculations, and comparisons as outlined below.

read point-by-point responses

Referee: [Abstract] Abstract: the statement that 'the corresponding haloes may collapse in heavier black holes which may form the entirety of the dark matter' is presented without any derivation of the minimum clustering strength, overdensity threshold, or collapse timescale relative to the evaporation time. This assumption is load-bearing for the entire proposal.

Authors: We acknowledge that this is a central assumption and that the abstract (and manuscript) would benefit from explicit support. In the revised version we will add a dedicated section providing order-of-magnitude estimates for the minimum clustering strength, the required overdensity threshold for halo collapse, and the collapse timescale relative to the PBH evaporation time. These estimates will be grounded in existing literature on PBH clustering and gravitational collapse, together with simple analytic arguments showing that the mechanism can operate before evaporation completes for sufficiently clustered initial conditions. revision: yes
Referee: [Abstract] Abstract: the claim that the scenario produces 'a flat stochastic background of gravitational waves which is detectable by the Einstein Telescope' is asserted without a spectrum calculation, strain amplitude estimate, frequency range, or comparison to the ET noise curve. No equation or figure supports the flatness or the detectability assertion.

Authors: We agree that the SGWB claim requires quantitative backing. In the revision we will include an explicit calculation of the stochastic gravitational-wave spectrum generated by the mergers within the collapsing haloes (or the associated dynamical processes), provide the characteristic strain amplitude as a function of frequency, specify the relevant frequency band, and overlay the predicted spectrum on the Einstein Telescope noise curve. A new figure will be added to illustrate the flatness of the spectrum and its position relative to ET sensitivity. revision: yes

Circularity Check

0 steps flagged

No significant circularity; scenario proposal rests on external assumptions rather than self-referential derivation

full rationale

The paper advances a qualitative scenario: strongly clustered light PBHs form haloes that collapse into heavier BHs comprising all DM, producing a detectable flat SGWB for ET. No equations, fitted parameters, power spectra, or collapse thresholds appear in the provided abstract, and the central claim is framed as an indirect signal under stated assumptions rather than a closed derivation. Without load-bearing steps that reduce by construction to the paper's own inputs (e.g., no self-citation of uniqueness theorems or fitted inputs renamed as predictions), the argument remains self-contained against external benchmarks such as clustering models and GW production calculations from the literature.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Review is abstract-only, so the ledger records only the explicit assumptions stated in the abstract. The scenario requires strong clustering and subsequent halo collapse to heavier black holes that comprise all dark matter; no free parameters or new entities are named in the abstract.

axioms (2)

domain assumption Primordial black holes can form in strongly clustered configurations.
Invoked to enable halo collapse into heavier black holes.
ad hoc to paper Collapsed haloes produce heavier black holes that can constitute the entirety of dark matter.
Central premise of the dark-matter claim; not derived in the abstract.

pith-pipeline@v0.9.0 · 5358 in / 1315 out tokens · 50346 ms · 2026-05-10T18:09:15.559342+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith/Foundation/RealityFromDistinction.lean reality_from_one_distinction unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

The indirect signal of such scenario is the production of a flat stochastic background of gravitational waves which is detectable by the Einstein Telescope.
IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

h²Ω_GW(f) = ... ∫ dt ds ... P_ζg[k √3/2 (s+t)] P_ζg[k √3/2 (s-t)]

What do these tags mean?

matches: The paper's claim is directly supported by a theorem in the formal canon.
supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

86 extracted references · 78 canonical work pages

[1]

Carr and S.W

B.J. Carr and S.W. Hawking,Black holes in the early Universe,Mon. Not. Roy. Astron. Soc. 168(1974) 399

1974
[2]

Carr,The Primordial black hole mass spectrum,Astrophys

B.J. Carr,The Primordial black hole mass spectrum,Astrophys. J.201(1975) 1

1975
[3]

Primordial black holes: constraints, potential evidence and prospects,

B. Carr, A.J. Iovino, G. Perna, V. Vaskonen and H. Veerm¨ ae,Primordial black holes: constraints, potential evidence and prospects,2601.06024

work page arXiv
[4]

Dom` enech, Universe7, 398 (2021), arXiv:2109.01398 [gr-qc]

G. Dom` enech,Scalar Induced Gravitational Waves Review,Universe7(2021) 398 [2109.01398]. [5]LISA Cosmology Working Groupcollaboration,Cosmology with the Laser Interferometer Space Antenna,Living Rev. Rel.26(2023) 5 [2204.05434]

work page arXiv 2021
[5]

Bartolo, V

N. Bartolo, V. De Luca, G. Franciolini, A. Lewis, M. Peloso and A. Riotto,Primordial Black Hole Dark Matter: LISA Serendipity,Phys. Rev. Lett.122(2019) 211301 [1810.12218]

work page arXiv 2019
[6]

Bartolo, V

N. Bartolo, V. De Luca, G. Franciolini, M. Peloso, D. Racco and A. Riotto,Testing primordial black holes as dark matter with LISA,Phys. Rev. D99(2019) 103521 [1810.12224]. [8]LISA Cosmology Working Groupcollaboration,Gravitational waves from inflation in LISA: reconstruction pipeline and physics interpretation,JCAP11(2024) 032 [2407.04356]. [9]LISA Cosmol...

work page arXiv 2019
[7]

Iovino, Junior., G

A. Iovino, Junior., G. Perna and H. Veerm¨ ae,The impact of non-Gaussianity when searching for Primordial Black Holes with LISA,2512.13648

work page arXiv
[8]

Punturo et al.,The Einstein Telescope: A third-generation gravitational wave observatory, Class

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

2010
[9]

Maggiore, C

M. Maggiore et al.,Science Case for the Einstein Telescope,JCAP03(2020) 050 [1912.02622]. [13]ETcollaboration,The Science of the Einstein Telescope,2503.12263

work page arXiv 2020
[10]

Chisholm,Clustering of primordial black holes: basic results,Phys

J.R. Chisholm,Clustering of primordial black holes: basic results,Phys. Rev. D73(2006) 083504 [astro-ph/0509141]

work page arXiv 2006
[11]

Tada and S

Y. Tada and S. Yokoyama,Primordial black holes as biased tracers,Phys. Rev. D91(2015) 123534 [1502.01124]

work page arXiv 2015
[12]

Ballesteros, P

G. Ballesteros, P.D. Serpico and M. Taoso,On the merger rate of primordial black holes: effects of nearest neighbours distribution and clustering,JCAP10(2018) 043 [1807.02084]

work page arXiv 2018
[13]

Belotsky, V.I

K.M. Belotsky, V.I. Dokuchaev, Y.N. Eroshenko, E.A. Esipova, M.Y. Khlopov, L.A. Khromykh et al.,Clusters of primordial black holes,Eur. Phys. J. C79(2019) 246 [1807.06590]

work page arXiv 2019
[14]

Desjacques and A

V. Desjacques and A. Riotto,Spatial clustering of primordial black holes,Phys. Rev. D98 (2018) 123533 [1806.10414]

work page arXiv 2018
[15]

Ali-Ha¨ ımoud,Correlation Function of High-Threshold Regions and Application to the Initial Small-Scale Clustering of Primordial Black Holes,Phys

Y. Ali-Ha¨ ımoud,Correlation Function of High-Threshold Regions and Application to the Initial Small-Scale Clustering of Primordial Black Holes,Phys. Rev. Lett.121(2018) 081304 [1805.05912]. – 13 –

work page arXiv 2018
[16]

Inman and Y

D. Inman and Y. Ali-Ha¨ ımoud,Early structure formation in primordial black hole cosmologies, Phys. Rev. D100(2019) 083528 [1907.08129]

work page arXiv 2019
[17]

Suyama and S

T. Suyama and S. Yokoyama,Clustering of primordial black holes with non-Gaussian initial fluctuations,PTEP2019(2019) 103E02 [1906.04958]

work page arXiv 2019
[18]

Matsubara, T

T. Matsubara, T. Terada, K. Kohri and S. Yokoyama,Clustering of primordial black holes formed in a matter-dominated epoch,Phys. Rev. D100(2019) 123544 [1909.04053]

work page arXiv 2019
[19]

Moradinezhad Dizgah, G

A. Moradinezhad Dizgah, G. Franciolini and A. Riotto,Primordial Black Holes from Broad Spectra: Abundance and Clustering,JCAP11(2019) 001 [1906.08978]

work page arXiv 2019
[20]

Young and C

S. Young and C.T. Byrnes,Initial clustering and the primordial black hole merger rate,JCAP 03(2020) 004 [1910.06077]

work page arXiv 2020
[21]

V. Atal, A. Sanglas and N. Triantafyllou,LIGO/Virgo black holes and dark matter: The effect of spatial clustering,JCAP11(2020) 036 [2007.07212]

work page arXiv 2020
[22]

De Luca, V

V. De Luca, V. Desjacques, G. Franciolini and A. Riotto,The clustering evolution of primordial black holes,JCAP11(2020) 028 [2009.04731]

work page arXiv 2020
[23]

De Luca, G

V. De Luca, G. Franciolini and A. Riotto,Constraining the initial primordial black hole clustering with CMB distortion,Phys. Rev. D104(2021) 063526 [2103.16369]

work page arXiv 2021
[24]

Gorton and A.M

M. Gorton and A.M. Green,Effect of clustering on primordial black hole microlensing constraints,2203.04209

work page arXiv
[25]

Petaˇ c, J

M. Petaˇ c, J. Lavalle and K. Jedamzik,Microlensing constraints on clustered primordial black holes,Phys. Rev. D105(2022) 083520 [2201.02521]

work page arXiv 2022
[26]

De Luca, G

V. De Luca, G. Franciolini and A. Riotto,Heavy Primordial Black Holes from Strongly Clustered Light Black Holes,Phys. Rev. Lett.130(2023) 171401 [2210.14171]

work page arXiv 2023
[27]

Animali and V

C. Animali and V. Vennin,Clustering of primordial black holes from quantum diffusion during inflation,JCAP08(2024) 026 [2402.08642]

work page arXiv 2024
[28]

Auclair and B

P. Auclair and B. Blachier,Small-scale clustering of primordial black holes: Cloud-in-cloud and exclusion effects,Phys. Rev. D109(2024) 123538 [2402.00600]

work page arXiv 2024
[29]

Crescimbeni, V

F. Crescimbeni, V. Desjacques, G. Franciolini, A. Ianniccari, A.J. Iovino, G. Perna et al.,The irrelevance of primordial black hole clustering in the LVK mass range,JCAP05(2025) 001 [2502.01617]

work page arXiv 2025
[30]

Black hole formation in the Friedmann universe: Formulation and computation in numerical relativity

M. Shibata and M. Sasaki,Black hole formation in the Friedmann universe: Formulation and computation in numerical relativity,Phys. Rev. D60(1999) 084002 [gr-qc/9905064]

work page Pith review arXiv 1999
[31]

Cosmological long-wavelength solutions and primordial black hole formation

T. Harada, C.-M. Yoo, T. Nakama and Y. Koga,Cosmological long-wavelength solutions and primordial black hole formation,Phys. Rev. D91(2015) 084057 [1503.03934]

work page Pith review arXiv 2015
[32]

Bardeen, J.R

J.M. Bardeen, J.R. Bond, N. Kaiser and A.S. Szalay,The Statistics of Peaks of Gaussian Random Fields,Astrophys. J.304(1986) 15

1986
[33]

Bardeen, J.R

J.M. Bardeen, J.R. Bond, N. Kaiser and A.S. Szalay,The Statistics of Peaks of Gaussian Random Fields,apj304(1986) 15

1986
[34]

V. Atal, J. Garriga and A. Marcos-Caballero,Primordial black hole formation with non-Gaussian curvature perturbations,JCAP09(2019) 073 [1905.13202]

work page arXiv 2019
[35]

Sasaki, J

M. Sasaki, J. Valiviita and D. Wands,Non-Gaussianity of the primordial perturbation in the curvaton model,Phys. Rev. D74(2006) 103003 [astro-ph/0607627]

work page arXiv 2006
[36]

Pi and M

S. Pi and M. Sasaki,Logarithmic Duality of the Curvature Perturbation,Phys. Rev. Lett.131 (2023) 011002 [2211.13932]

work page arXiv 2023
[37]

Atal and C

V. Atal and C. Germani,The role of non-gaussianities in Primordial Black Hole formation, Phys. Dark Univ.24(2019) 100275 [1811.07857]. – 14 –

work page arXiv 2019
[38]

Karam, N

A. Karam, N. Koivunen, E. Tomberg, V. Vaskonen and H. Veerm¨ ae,Anatomy of single-field inflationary models for primordial black holes,JCAP03(2023) 013 [2205.13540]

work page arXiv 2023
[39]

Inflationary interpretation of the nHz gravitational-wave background,

L. Frosina and A. Urbano,Inflationary interpretation of the nHz gravitational-wave background,Phys. Rev. D108(2023) 103544 [2308.06915]

work page arXiv 2023
[40]

D.H. Lyth, C. Ungarelli and D. Wands,The Primordial density perturbation in the curvaton scenario,Phys. Rev. D67(2003) 023503 [astro-ph/0208055]

work page arXiv 2003
[41]

Enqvist and S

K. Enqvist and S. Nurmi,Non-gaussianity in curvaton models with nearly quadratic potential, JCAP10(2005) 013 [astro-ph/0508573]

work page arXiv 2005
[42]

Lyth,Non-gaussianity and cosmic uncertainty in curvaton-type models,JCAP06(2006) 015 [astro-ph/0602285]

D.H. Lyth,Non-gaussianity and cosmic uncertainty in curvaton-type models,JCAP06(2006) 015 [astro-ph/0602285]

work page arXiv 2006
[43]

K. Ando, M. Kawasaki and H. Nakatsuka,Formation of primordial black holes in an axionlike curvaton model,Phys. Rev. D98(2018) 083508 [1805.07757]

work page arXiv 2018
[44]

Primordial black holes in the curvaton model: possible connections to pulsar timing arrays and dark matter,

G. Ferrante, G. Franciolini, A. Iovino, Junior. and A. Urbano,Primordial black holes in the curvaton model: possible connections to pulsar timing arrays and dark matter,JCAP06(2023) 057 [2305.13382]

work page arXiv 2023
[45]

Kolb and I.I

E.W. Kolb and I.I. Tkachev,Large amplitude isothermal fluctuations and high density dark matter clumps,Phys. Rev. D50(1994) 769 [astro-ph/9403011]

work page arXiv 1994
[46]

De Luca, G

V. De Luca, G. Franciolini, A. Riotto and H. Veerm¨ ae,Ruling out Initial Primordial Black Hole Clustering,Phys. Rev. Lett.(2022) [2208.01683]

work page arXiv 2022
[47]

Kolb and I.I

E.W. Kolb and I.I. Tkachev,Axion miniclusters and Bose stars,Phys. Rev. Lett.71(1993) 3051 [hep-ph/9303313]

work page arXiv 1993
[48]

Misner, K.S

C.W. Misner, K.S. Thorne and J.A. Wheeler,Gravitation, W. H. Freeman, San Francisco (1973)

1973
[49]

Primordial Black Holes - Perspectives in Gravitational Wave Astronomy -

M. Sasaki, T. Suyama, T. Tanaka and S. Yokoyama,Primordial black holes—perspectives in gravitational wave astronomy,Class. Quant. Grav.35(2018) 063001 [1801.05235]

work page Pith review arXiv 2018
[50]

Binney and S

J. Binney and S. Tremaine,Galactic dynamics, Princeton University Press (1987)

1987
[51]

Arbey, J

A. Arbey, J. Auffinger and J. Silk,Evolution of primordial black hole spin due to Hawking radiation,Mon. Not. Roy. Astron. Soc.494(2020) 1257 [1906.04196]

work page arXiv 2020
[52]

Leach, M

S.M. Leach, M. Sasaki, D. Wands and A.R. Liddle,Enhancement of superhorizon scale inflationary curvature perturbations,Phys. Rev. D64(2001) 023512 [astro-ph/0101406]

work page arXiv 2001
[53]

Franciolini and A

G. Franciolini and A. Urbano,Primordial black hole dark matter from inflation: The reverse engineering approach,Phys. Rev. D106(2022) 123519 [2207.10056]

work page arXiv 2022
[54]

Tomita,Evolution of Irregularities in a Chaotic Early Universe,Prog

K. Tomita,Evolution of Irregularities in a Chaotic Early Universe,Prog. Theor. Phys.54 (1975) 730

1975
[55]

Matarrese, O

S. Matarrese, O. Pantano and D. Saez,General relativistic dynamics of irrotational dust: Cosmological implications,Phys. Rev. Lett.72(1994) 320 [astro-ph/9310036]

work page arXiv 1994
[56]

Acquaviva, N

V. Acquaviva, N. Bartolo, S. Matarrese and A. Riotto,Second order cosmological perturbations from inflation,Nucl. Phys. B667(2003) 119 [astro-ph/0209156]

work page arXiv 2003
[57]

Mollerach, D

S. Mollerach, D. Harari and S. Matarrese,CMB polarization from secondary vector and tensor modes,Phys. Rev. D69(2004) 063002 [astro-ph/0310711]

work page arXiv 2004
[58]

Ananda, C

K.N. Ananda, C. Clarkson and D. Wands,The Cosmological gravitational wave background from primordial density perturbations,Phys. Rev. D75(2007) 123518 [gr-qc/0612013]

work page arXiv 2007
[59]

Baumann, P.J

D. Baumann, P.J. Steinhardt, K. Takahashi and K. Ichiki,Gravitational Wave Spectrum Induced by Primordial Scalar Perturbations,Phys. Rev. D76(2007) 084019 [hep-th/0703290]. – 15 –

work page arXiv 2007
[60]

Iovino, G

A.J. Iovino, G. Perna, D. Perrone, D. Racco and A. Riotto,Understanding the nature of scalar-induced gravitational waves,JCAP03(2026) 001 [2509.24774]

work page arXiv 2026
[61]

A Cosmological Signature of the SM Higgs Instability: Gravitational Waves

J.R. Espinosa, D. Racco and A. Riotto,A Cosmological Signature of the SM Higgs Instability: Gravitational Waves,JCAP09(2018) 012 [1804.07732]

work page Pith review arXiv 2018
[62]

Y.-F. Cai, X. Chen, M.H. Namjoo, M. Sasaki, D.-G. Wang and Z. Wang,Revisiting non-Gaussianity from non-attractor inflation models,JCAP05(2018) 012 [1712.09998]

work page Pith review arXiv 2018
[63]

R.-g. Cai, S. Pi and M. Sasaki,Gravitational Waves Induced by non-Gaussian Scalar Perturbations,Phys. Rev. Lett.122(2019) 201101 [1810.11000]

work page arXiv 2019
[64]

Unal, Phys

C. Unal,Imprints of Primordial Non-Gaussianity on Gravitational Wave Spectrum,Phys. Rev. D99(2019) 041301 [1811.09151]

work page arXiv 2019
[65]

R.-G. Cai, S. Pi, S.-J. Wang and X.-Y. Yang,Pulsar Timing Array Constraints on the Induced Gravitational Waves,JCAP10(2019) 059 [1907.06372]

work page arXiv 2019
[66]

Hajkarim and J

F. Hajkarim and J. Schaffner-Bielich,Thermal History of the Early Universe and Primordial Gravitational Waves from Induced Scalar Perturbations,Phys. Rev. D101(2020) 043522 [1910.12357]

work page arXiv 2020
[67]

Atal and G

V. Atal and G. Dom` enech,Probing non-Gaussianities with the high frequency tail of induced gravitational waves,JCAP06(2021) 001 [2103.01056]

work page arXiv 2021
[68]

Yuan and Q.-G

C. Yuan and Q.-G. Huang,Gravitational waves induced by the local-type non-Gaussian curvature perturbations,Phys. Lett. B821(2021) 136606 [2007.10686]

work page arXiv 2021
[69]

Dom` enech, S

G. Dom` enech, S. Passaglia and S. Renaux-Petel,Gravitational waves from dark matter isocurvature,JCAP03(2022) 023 [2112.10163]

work page arXiv 2022
[70]

Garcia-Saenz, L

S. Garcia-Saenz, L. Pinol, S. Renaux-Petel and D. Werth,No-go theorem for scalar-trispectrum-induced gravitational waves,JCAP03(2023) 057 [2207.14267]

work page arXiv 2023
[71]

Implications for the non-Gaussianity of curvature perturbation from pulsar timing arrays,

L. Liu, Z.-C. Chen and Q.-G. Huang,Implications for the non-Gaussianity of curvature perturbation from pulsar timing arrays,Phys. Rev. D109(2024) L061301 [2307.01102]

work page arXiv 2024
[72]

Yuan, D.-S

C. Yuan, D.-S. Meng and Q.-G. Huang,Full analysis of the scalar-induced gravitational waves for the curvature perturbation with local-type non-Gaussianities,JCAP12(2023) 036 [2308.07155]

work page arXiv 2023
[73]

J.-P. Li, S. Wang, Z.-C. Zhao and K. Kohri,Complete analysis of the background and anisotropies of scalar-induced gravitational waves: primordial non-Gaussianity f N L and g N L considered,JCAP06(2024) 039 [2309.07792]

work page arXiv 2024
[74]

Adshead, K

P. Adshead, K.D. Lozanov and Z.J. Weiner,Non-Gaussianity and the induced gravitational wave background,JCAP10(2021) 080 [2105.01659]

work page arXiv 2021
[75]

Perna, C

G. Perna, C. Testini, A. Ricciardone and S. Matarrese,Fully non-Gaussian Scalar-Induced Gravitational Waves,JCAP05(2024) 086 [2403.06962]

work page arXiv 2024
[76]

R. Inui, C. Joana, H. Motohashi, S. Pi, Y. Tada and S. Yokoyama,Primordial black holes and induced gravitational waves from logarithmic non-Gaussianity,JCAP03(2025) 021 [2411.07647]

work page arXiv 2025
[77]

Iovino, G

A.J. Iovino, G. Perna, A. Riotto and H. Veerm¨ ae,Curbing PBHs with PTAs,JCAP10(2024) 050 [2406.20089]

work page arXiv 2024
[78]

Iovino, S

A.J. Iovino, S. Matarrese, G. Perna, A. Ricciardone and A. Riotto,How well do we know the scalar-induced gravitational waves?,Phys. Lett. B872(2026) 140039 [2412.06764]

work page arXiv 2026
[79]

Foster, D

J.W. Foster, D. Blas, A. Bourgoin, A. Hees, M. Herrero-Valea, A.C. Jenkins et al.,Discovering µHz gravitational waves and ultra-light dark matter with binary resonances,2504.15334. – 16 –

work page arXiv
[80]

Chambers, K.C.,et al.2016,arXiv e-prints, arXiv:1612.05560

D. Blas, J.W. Foster, Y. Gouttenoire, A.J. Iovino, I. Musco, S. Trifinopoulos et al.,The Dark Side of the Moon: Listening to Scalar-Induced Gravitational Waves,2602.12252. [85]LISAcollaboration,New horizons for fundamental physics with LISA,Living Rev. Rel.25 (2022) 4 [2205.01597]

work page arXiv 2022

Showing first 80 references.