{"total":24,"items":[{"citing_arxiv_id":"2605.27910","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Matching second-order classical and 1-loop quantum tensor power spectra in de Sitter spacetime","primary_cat":"hep-ph","submitted_at":"2026-05-27T03:36:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Classical part of 1-loop tensor power spectrum in de Sitter is IR divergent but cancels with vacuum part, enabling non-perturbative renormalization to extract unaffected physical information.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27231","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Fast Method to Compute Scalar Induced Gravitational Waves on a Lattice with Primordial Non-Gaussianities","primary_cat":"astro-ph.CO","submitted_at":"2026-05-26T16:11:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A new lattice method recasts SIGW integrals as FFT convolutions to compute fully non-Gaussian spectra in seconds with ~10% error on a radiation-dominated background.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21477","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Opening the Window of Ultra-Light PBHs by Exorcising the Poltergeist","primary_cat":"hep-ph","submitted_at":"2026-05-20T17:57:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Incorporating the general-relativity mass tail df_PBH/d ln M ∝ M^3.78 smooths PBH evaporation, suppresses the scalar-induced GW signal by orders of magnitude, and reopens the ultra-light PBH window for the hot Big Bang.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21474","ref_index":192,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational Waves from Black Hole Reheating: The Scalar-Induced Component","primary_cat":"hep-ph","submitted_at":"2026-05-20T17:55:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Accounting for the minimal mass spread of primordial black holes from gravitational collapse suppresses the Poltergeist GW background to the level of generic scalar-induced signals and reopens ultra-light PBH parameter space.","context_count":1,"top_context_role":"baseline","top_context_polarity":"support","context_text":"Fork < k reh, the modes enter the horizon only after PBH evaporation and are therefore insensitive to both the intermediate PBH era and PBH isocurvature perturbations. The resulting signal reduces to the standard radiation-era contribution, Ω(RD2,irred.) GW [S] = 0,Ω (RD2,irred.) GW = Ω(RD2,irred.) GW [Φ],(125) already present in the absence of PBHs [192, 194, 298]. We refer to this unavoidable component as theirreduciblegravitational-wave background. 2.Ω (eMD) GW (Sec. 6): SIGWs sourced during the PBH-dominated era, where the gravita- tional potential remains approximately constant [194]. Both adiabatic and isocurvature contributions are included, Ω(eMD) GW = Ω(eMD) GW [Φ] + Ω(eMD) GW [S].(126) The adiabatic component has been studied for constant and time-dependent decay rates [196-"},{"citing_arxiv_id":"2605.11956","ref_index":47,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing the small-scale primordial power spectrum via relic neutrinos and acoustic reheating","primary_cat":"hep-ph","submitted_at":"2026-05-12T11:08:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Dissipation of small-scale primordial perturbations after neutrino decoupling cools relic neutrinos and reduces their abundance, enabling PTOLEMY to constrain the primordial curvature power spectrum to O(0.1) on scales k ≲ 3×10^5 Mpc^{-1}.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"sidering a sharpmonochromatic peak, which is an ideal- ized description of models where perturbations are am- plified on a very narrow range of scales. This can arise in models featuring brief violations of slow-roll or non- attractor phases, turns in multi-field inflationary trajec- tories, and particle production [42-46], and is a useful and widely adopted benchmark [47, 48]. We parametrize this as ∆ 2 R(k) =αk ⋆δ(k−k ⋆), withαcontrolling the amplitude of the enhancement at the scalek ⋆. Amplification phases of finite duration are naturally captured by abroad peaktemplate. Such phases occur e.g. in single-field models with inflection points leading to ultra-slow-roll dynamics during which curvature pertur- bations are amplified."},{"citing_arxiv_id":"2605.04154","ref_index":48,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Master Equation for Screening in Luminal Horndeski Gravity","primary_cat":"gr-qc","submitted_at":"2026-05-05T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A master screening equation is derived for luminal Horndeski gravity that recovers Vainshtein and Chameleon mechanisms and introduces Phaedrus screening with screening radius scaling linearly with source mass.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"this is driven exclusively by the cubic Galileon and thus fully described by quadratic nonlinearities. Second, it also provides an effective description of Chameleon screening by captur- ing the leading-order shift in the scalar's effective mass, even though formally resolving the exact thin-shell profile requires 2 This degeneracy is termed 'permanent underdetermination' (see [48] for a taxonomy of potential resolutions). Alongside complementary tests in strong gravity regimes, as is possible e.g. in the context of black hole quasi- normal modes in [49], the screening identification framework presented in this work can provide a way to discriminate between otherwise identical theories. 3 Note that we consider exclusively scalar perturbations of the metric, assum-"},{"citing_arxiv_id":"2604.25726","ref_index":22,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Imprint of domain wall annihilation on induced gravitational waves","primary_cat":"hep-ph","submitted_at":"2026-04-28T14:53:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Domain wall annihilation imprints a two-peaked spectrum on induced gravitational waves via an early matter-dominated phase and entropy dilution.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"bations interact at second-order to produce GWs. The resulting IGW spectrum carries information about small- scale scalar perturbations and provides an independent window into primordial Universe. Interestingly, if the Universe proceeds through an era of early MD following the initial radiation domination after reheating, the pro- duction of such IGWs gets intensified [22, 23, 74-86] but the accurate estimation of such spectrum are challenging [85, 86]. The degree of enhancement depends on whether perturbations evolve linearly or non-linearly. In the lin- earregime[77-79], whereperturbationsremainsmalland analytical or semi-analytical methods reliably estimate IGW production, one expects moderate enhancement of the IGW spectrum."},{"citing_arxiv_id":"2604.22731","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Precision Analysis for $\\boldsymbol{H_0}$ Using Upcoming Multi-band Gravitational Wave Observations","primary_cat":"astro-ph.CO","submitted_at":"2026-04-24T17:28:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Multi-band GW observations of PBHs can reduce H0 uncertainty to ≲2 km/s/Mpc (conservative) or O(0.1) km/s/Mpc (optimistic) via Fisher forecasts on M_PBH and f_PBH.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Kavanagh,Primordial Black Holes as a dark matter candidate,J. Phys. G48(2021) 043001 [2007.10722]. [18] B. Carr and F. 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Lett.117(2016) 061101 [1603."},{"citing_arxiv_id":"2604.22634","ref_index":46,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraints on the Primordial Black Hole Abundance using Pulsar Parameter Drifts","primary_cat":"astro-ph.CO","submitted_at":"2026-04-24T15:07:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"The first search for scalar-induced gravitational waves via pulsar parameter drifts yields f_PBH < 10^{-10} (95% CL) for PBH masses 0.3 to 4e4 solar masses, strongly disfavoring a primordial black hole origin for LVK binary black holes.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"and Kazunori Kohri, \"Cosmic microwave background bounds on primordial black holes including dark mat- ter halo accretion,\" Phys. Rev. Res.2, 023204 (2020), arXiv:2002.10771 [astro-ph.CO]. [45] Kishore N. Ananda, Chris Clarkson, and David Wands, \"The Cosmological gravitational wave background from primordial density perturbations,\" Phys. Rev. D75, 123518 (2007), arXiv:gr-qc/0612013. [46] Daniel Baumann, Paul J. Steinhardt, Keitaro Takahashi, and Kiyotomo Ichiki, \"Gravitational Wave Spectrum In- duced by Primordial Scalar Perturbations,\" Phys. Rev. D76, 084019 (2007), arXiv:hep-th/0703290. [47] Ryo Saito and Jun'ichi Yokoyama, \"Gravitational wave background as a probe of the primordial black hole abun- dance,\" Phys. Rev. Lett.102, 161101 (2009), [Erratum:"},{"citing_arxiv_id":"2604.21642","ref_index":53,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Exploring the statistical anisotropy of primordial curvature perturbations with pulsar timing arrays","primary_cat":"gr-qc","submitted_at":"2026-04-23T12:57:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A phenomenological dipole anisotropy in primordial perturbations induces dipolar and quadrupolar anisotropies in SIGW energy density spectra, producing frequency-dependent PTA overlap reduction functions that depend on pulsar sky distribution, but NANOGrav 15-year data yields no significant evidence","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"D111, 075034 (2025), arXiv:2408.15912 [hep-ph]. [50] S. Jiang, F. P. Huang, and C. S. Li, Phys. Rev. D108, 063508 (2023), arXiv:2305.02218 [hep-ph]. [51] R.-G. Cai, S.-J. Wang, and Z.-Y. Yuwen, Phys. Rev. D108, L021502 (2023), arXiv:2305.00074 [gr-qc]. [52] J. Liu, L. Bian, R.-G. Cai, Z.-K. Guo, and S.-J. Wang, Phys. Rev. Lett.130, 051001 (2023), arXiv:2208.14086 [astro-ph.CO]. [53] K. N. Ananda, C. Clarkson, and D. Wands, Phys. Rev. D75, 123518 (2007), arXiv:gr-qc/0612013. [54] D. Baumann, P. J. Steinhardt, K. Takahashi, and K. Ichiki, Phys. Rev. D76, 084019 (2007), arXiv:hep-th/0703290. [55] J. R. Espinosa, D. Racco, and A. Riotto, JCAP09, 012 (2018), arXiv:1804.07732 [hep-ph]. [56] K. Kohri and T. Terada, Phys. Rev. D97, 123532 (2018), arXiv:1804."},{"citing_arxiv_id":"2604.20063","ref_index":49,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Purely Quadratic Non-Gaussianity from Tachyonic Instability: Primordial Black Holes and Scalar-Induced Gravitational Waves","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T23:58:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Purely quadratic non-Gaussianity from tachyonic instability allows narrow curvature spectra to exponentially suppress primordial black hole overproduction via correlation coefficient ρ approaching -1 while retaining sizable scalar-induced gravitational waves.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"72, 320 (1994), arXiv:astro-ph/9310036. [47] V. Acquaviva, N. Bartolo, S. Matarrese, and A. Riotto, Second order cosmological perturbations from inflation, Nucl. Phys. 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D76, 084019 (2007), arXiv:hep-th/0703290."},{"citing_arxiv_id":"2604.15313","ref_index":157,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational-wave lensing beyond rays: a disordered-system approach","primary_cat":"astro-ph.CO","submitted_at":"2026-04-16T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A quenched-disorder approach with Schwinger-Keldysh path integrals produces an averaged density matrix for gravitational waves that separates phase-suppressing exponential terms from oscillatory corrections to coherent propagation.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"24) is relevant for our purposes, since our final results will depend only on the square modulus of this contribution. The two sums in Eq. (4.24) can be resummed +∞X n=1 n2 (n2 −a 2) = 1 2 − aπ 2 cot(πa) + +∞X n=1 1,(4.27) +∞X n=1 n4 (n2 −a 2)(n2 −b 2) = 1 2 + b3πcot(πb)−a 3πcot(πa) 2(a2 −b 2) + +∞X n=1 1,(4.28) where we have used the Mittag-Leffler [157] expansion for cotangent function. This resumma- tion makes explicit the diverging factor (last contribution), which however can be reabsorbed in the normalization of the time evolution operator. The resummed version of Eq. (4.24), obtained using these identities, coincides with the expression of the loop correction computed with the resummed propagator of Eq."},{"citing_arxiv_id":"2604.15219","ref_index":24,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Nonperturbative stochastic inflation in perturbative dynamical background","primary_cat":"astro-ph.CO","submitted_at":"2026-04-16T16:50:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Derives stochastic equations from Schwinger-Keldysh formalism that include quantum diffusion and classical metric perturbations for non-perturbative ultra-slow-roll inflation, validated on Starobinsky and critical Higgs models.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"D97, 123532 (2018), arXiv:1804.08577 [gr-qc]. [22] Jos' e Ram' on Espinosa, Davide Racco, and Antonio Riotto, \"A Cosmological Signature of the SM Higgs Instability: Gravitational Waves,\" JCAP09, 012 (2018), arXiv:1804.07732 [hep-ph]. [23] Guillem Dom` enech, \"Scalar Induced Gravitational Waves Review,\" Universe7, 398 (2021), arXiv:2109.01398 [gr-qc]. [24] Rong-Gen Cai, Shi Pi, and Misao Sasaki, \"Gravitational Waves Induced by non-Gaussian Scalar Perturbations,\" Phys. Rev. Lett.122, 201101 (2019), arXiv:1810.11000 [astro-ph.CO]. [25] Caner Unal, \"Imprints of Primordial Non-Gaussianity on Gravitational Wave Spectrum,\" Phys. Rev. D99, 041301 (2019), arXiv:1811.09151 [astro-ph.CO]. [26] Peter Adshead, Kaloian D."},{"citing_arxiv_id":"2604.08493","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing non-Gaussianity during reheating with SIGW in the LISA band","primary_cat":"astro-ph.CO","submitted_at":"2026-04-09T17:34:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Non-standard reheating imprints detectable features on SIGW spectra via non-Gaussianity, with dynamics that can suppress or boost the signal amplitude for LISA.","context_count":1,"top_context_role":"other","top_context_polarity":"unclear","context_text":"[13]ETcollaboration,Science Case for the Einstein Telescope,JCAP03(2020) 050 [1912.02622]. [14]ETcollaboration,The Science of the Einstein Telescope,2503.12263. [15] D. Reitze et al.,Cosmic Explorer: The U.S. Contribution to Gravitational-Wave Astronomy beyond LIGO,Bull. Am. Astron. Soc.51(2019) 035 [1907.04833]. 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Tomita,Non-Linear Theory of Gravitational Instability in the Expanding Universe,Prog."},{"citing_arxiv_id":"2604.06082","ref_index":58,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Hunting Dark Matter with the Einstein Telescope","primary_cat":"astro-ph.CO","submitted_at":"2026-04-07T17:00:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Clustered primordial black holes may constitute all dark matter and produce a flat stochastic gravitational wave background detectable by the Einstein Telescope.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"494(2020) 1257 [1906.04196]. [56] 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]. [57] G. Franciolini and A. 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Riotto,Second order cosmological perturbations"},{"citing_arxiv_id":"2604.05078","ref_index":98,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational Waves from Matter Perturbations of Spectator Scalar Fields","primary_cat":"hep-ph","submitted_at":"2026-04-06T18:29:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A spectator scalar field with strong portal coupling to the inflaton sources a stochastic gravitational wave background reaching Ω_GW h² ∼ 10^{-11} at frequencies 10^7-10^8 Hz for benchmark parameters σ/λ ≃ 10^4 and T_reh = 2×10^{14} GeV.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"This turbulent cascade is visible in the right panel of Fig. 2 as the enhanced late-time amplitude of the translucent (lattice) curves relative to the opaque (Hartree) ones, particularly forλ χ = 10−3. A systematic comparison between the quantum 2PI Hartree truncation and classical lattice simulations for a self-interacting spectator was performed in Refs. [98, 99], whereO(1) agreement in the final two-point function was found, along with a novel nonlinear resonance driven by⟨χ 2⟩that can dominate the total particle yield. Similar behavior has been observed in lattice studies of non-minimally coupled spectators, where the self-interaction regularizes the tachyonic growth while simultaneously feeding a turbulent"},{"citing_arxiv_id":"2512.08301","ref_index":31,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Isocurvature Induced Gravitational Waves at Pulsar Timing Arrays","primary_cat":"astro-ph.CO","submitted_at":"2025-12-09T07:00:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The work shows that free-streaming dark radiation isocurvature produces a qualitatively different gravitational wave spectrum than cold dark matter isocurvature and derives constraints on isocurvature power spectra around 10^6 Mpc^{-1} from NANOGrav data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.05967","ref_index":81,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Stochastic Gravitational Waves from Modulated Reheating","primary_cat":"astro-ph.CO","submitted_at":"2025-10-07T14:23:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A spectator scalar in modulated reheating with large Higgs-like couplings generates detectable scalar-induced stochastic gravitational waves for BBO and DECIGO, but only outside perturbative low-energy extrapolations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.10812","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Scalar-induced gravitational waves with non-Gaussianity up to all orders","primary_cat":"astro-ph.CO","submitted_at":"2025-08-14T16:38:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Lattice simulations directly calculate SIGW spectra with non-Gaussianity to all orders and show that modest non-Gaussianity alters ultraviolet spectral behavior.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.09552","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing the scalar-induced gravitational waves with the Five-hundred-meter Aperture Spherical radio Telescope and the Square Kilometer Array","primary_cat":"astro-ph.CO","submitted_at":"2025-07-13T09:38:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Forecasts show that adding FAST/SKA upper or lower limits on scalar-induced GWs to CMB+BAO data shifts the scalar spectral index ns by several sigma in LambdaCDM+r and extended models, offering a potential detection indicator.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.16820","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Isotropy, anisotropies and non-Gaussianity in the scalar-induced gravitational-wave background: diagrammatic approach for primordial non-Gaussianity up to arbitrary order","primary_cat":"astro-ph.CO","submitted_at":"2025-05-22T15:55:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Extends diagrammatic approach for scalar-induced gravitational waves to arbitrary-order local PNG, deriving semi-analytic spectra for energy density, anisotropies, bispectrum and trispectrum up to quartic terms.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"diagram vanishes, and all loop 3-momenta should be integrated over. In particular, while vertices with identical solid-line counts but distinct red-line counts are treated as distinct en- tities, we assign them the same PNG parameters. This treatment is consistent, as our present analysis is confined to the scale-independent PNG scenario. Specifically, according to Fig. 1, while the Gaussian-vertex meansV [1] 0 = 1 by definition, we introduce theF NL-vertices with V [2] 0 =V [2] 1 =F NL, theG NL-vertices withV [3] 0 =V [3] 1 =V [3] 2 =G NL, and theH NL-vertices withV [4] 0 =V [4] 1 =V [4] 2 =V [4] 3 =H NL. Utilizing these Feynman-like rules, we can draw diagrams that representωgw,in and its multi-point correlators. The various configurations of - 12 -"},{"citing_arxiv_id":"2504.11275","ref_index":48,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Relic gravitational waves from primordial gravitational collapses","primary_cat":"gr-qc","submitted_at":"2025-04-15T15:15:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Sound shell collisions from Hubble-scale primordial density perturbations generate a stochastic GW background whose peak frequency and amplitude scale with the Hubble horizon and shell abundance.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.01962","ref_index":46,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Curvature Perturbations from First-Order Phase Transitions: Implications to Black Holes and Gravitational Waves","primary_cat":"hep-ph","submitted_at":"2025-03-03T19:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Covariant analysis of curvature perturbations from first-order phase transitions reveals gauge-dependent overestimation of primordial black holes and gravitational waves in prior non-covariant calculations, leading to strong suppression of both signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2109.01398","ref_index":38,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Scalar induced gravitational waves review","primary_cat":"gr-qc","submitted_at":"2021-09-03T09:44:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review that unifies analytical expressions for scalar-induced gravitational waves and emphasizes calculations for non-radiation-dominated cosmologies.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"GWs in a dust dominated universe suffer from gauge ambiguities. They proceeded to argue that only the oscillating part of the induced tensor modes were identified astrue gravitational waves. We will discuss more about the gauge ambiguities in Sec. 7. However, Refs. [35-37] concluded that induced GWs were too small to be practically observed. It was not until 20 years later that Ananda, Clarkson and Wands [38] started to uncover the potential of induced GWs. In Ref. [38] they proposed to use induced GWs, generated in a radiation 1 INTRODUCTION page 5 of 98 dominated universe, to constrain the spectral tilt of primordial fluctuations. A blue tilted primordial spectrum even with theCMB normalization mightend upyieldinglarge enough inducedGWs. Some months later, Baumann, Steinhardt, Takahashi and Ichiki [39] looked into more detail at the transfer"}],"limit":50,"offset":0}