{"total":29,"items":[{"citing_arxiv_id":"2605.21477","ref_index":73,"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":239,"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":"method","top_context_polarity":"use_method","context_text":"wave background Ω(form) GW [Φ] at the horizon re-entry of the scalek f. We show the representative benchmark spectra in Fig. 16. 8.1 Spectrum at formation Inserting the log-normal curvature spectrum into the master formula (106) gives analytic ap- proximations for the SIGW spectrum at formation [312]. We use the dimensionless wavenumber κf ≡ k kf .(239) For broad spectra, ∆≳0.1, the result can be written as Ω(form) GW [Φ] A2 R ≃ 4κ3 f 5√π e9∆2/4 ∆ \"\"\u0012 lnκ f + 3∆2 2 \u00132 + ∆2 2 # erfc   ln \u0010p 3/2κ f \u0011 + 3∆2/2 ∆   − ∆√π exp  − \u0010 ln \u0010p 3/2κ f \u0011 + 3∆2/2 \u00112 ∆2   \u0014 ln \u0010p 2/3κ f \u0011 + 3∆2 2 \u0015# (240) + 0.0659 ∆2 κ2 f e∆2 exp  − \u0010 ∆2 + ln \u0010p 3/4κ f \u0011\u00112 ∆2   + 1 3 r 2 π κ−4 f e8∆2 ∆ exp \u0014 −ln2 κf"},{"citing_arxiv_id":"2605.21050","ref_index":62,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on Kaniadakis Cosmology from Starobinsky Inflation and Primordial Tensor Perturbations","primary_cat":"gr-qc","submitted_at":"2026-05-20T11:34:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Kaniadakis entropic cosmology modifies early-universe dynamics and is constrained by its predictions for Starobinsky inflation and the primordial tensor spectrum using current CMB and gravitational-wave observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20332","ref_index":95,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological History of Flavour Deconstruction Models: Constraints from Monopole Production","primary_cat":"hep-ph","submitted_at":"2026-05-19T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Flavour deconstruction models with semi-simple gauge groups generically produce light monopoles that require low-scale reheating after inflation to satisfy cosmological and astrophysical bounds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19336","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Recombination Thickness as an Uncertainty in Inflationary Observables","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T04:19:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Finite recombination thickness introduces Gaussian smoothing in ln k to the primordial power spectrum, producing non-trivial differences between TT and EE spectral indices that may be detectable in future CMB data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18286","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primary gravitational waves at high frequencies II: Emergence of the exponential cut-off in the power spectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-05-18T12:15:02+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"For infinitely differentiable effective potentials describing the post-inflation transition, the regularized power spectrum of primary gravitational waves exhibits exponential suppression at small scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15259","ref_index":134,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"TransitionListener v2.0 -- Robust gravitational wave predictions for cosmological phase transitions","primary_cat":"hep-ph","submitted_at":"2026-05-14T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"TransitionListener v2.0 supplies an end-to-end pipeline from scalar potential to gravitational wave spectra with improved handling of transition dynamics and bubble separation.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[132] B. Sathyaprakash et al. \"Scientific Objectives of Einstein Telescope\". In:Class. Quant. Grav.29 (2012). Ed. by Mark Hannam et al., p. 124013.doi:10.1088/0264-9381/29/1 2/124013. arXiv:1206.0331 [gr-qc]. 67 [133] J. Aasi et al. \"Advanced LIGO\". In:Class. Quant. Grav.32 (2015), p. 074001.doi: 10.1088/0264-9381/32/7/074001. arXiv:1411.4547 [gr-qc]. [134] F. Acernese et al. \"Advanced Virgo: a second-generation interferometric gravitational wave detector\". In:Class. Quant. Grav.32.2 (2015), p. 024001.doi:10.1088/0264-938 1/32/2/024001. arXiv:1408.3978 [gr-qc]. [135] Keiko Kokeyama. \"KAGRA, the underground and cryogenic laser interferometer for grav- itational wave detection\". In:14th Pacific Rim Conference on Lasers and Electro-Optics."},{"citing_arxiv_id":"2605.04487","ref_index":65,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational wave emission from nonspherical collapse in an early matter-dominated era using N-body simulations","primary_cat":"astro-ph.CO","submitted_at":"2026-05-06T04:31:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Full numerical N-body treatment is required for reliable gravitational wave predictions from nonspherical collapse in early matter-dominated eras, with resulting spectra mappable to detector sensitivities via horizon mass and reheating temperature.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Trh ≳4MeV to be consistent with the thermal history of the Universe, e.g., the BBN (Big- Bang Nucleosynthesis) and the CMB (Cosmic Microwave Background) [55-60] (see also a review article [1]). The comparison with detector sensitivities is shown in Fig. 13. The four panels cor- respond, respectively, to the frequency bands probed by pulsar timing arrays (NANOGrav [61], EPTA [62], IPTA [63], PPTA [64], and SKA [65]) 8 , space-based interferometers (Big Bang Observatory-BBO [69], LISA [70], DECIGO [71], TAIJI [72], TIANQIN [73] andµ-Ares [74]), ground-based interferometers LVK [75, 76], LIGO A + [77], Einstein Telescope [78], and Cosmic Explorer [79]), and high-frequency resonant-cavity searches [80, 81] (we take the sensitivity band from Ref. [82]). The numerical curves shown in each panel correspond to"},{"citing_arxiv_id":"2605.01992","ref_index":63,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Reviving Motivated Inflationary Potentials with $K$-inflation in the light of ACT","primary_cat":"gr-qc","submitted_at":"2026-05-03T17:48:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"K-inflation with non-canonical kinetic term G(φ) shifts α-attractor T-models and natural inflation into the Planck-ACT-LB-BK18 allowed region while satisfying Swampland conjectures and producing testable GW spectra.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[61]LIGO Scientific, VIRGO, KAGRAcollaboration,Cosmological and High Energy Physics 33 implications from gravitational-wave background searches in LIGO-Virgo-KAGRA's O1-O4a runs, 2510.26848. [62]LIGO Scientific, VIRGOcollaboration,Characterization of the LIGO detectors during their sixth science run,Class. Quant. Grav.32(2015) 115012 [1410.7764]. [63]LIGO Scientific, Virgocollaboration,Search for the isotropic stochastic background using data from Advanced LIGO's second observing run,Phys. Rev. D100(2019) 061101 [1903.02886]. [64]LISAcollaboration,Laser Interferometer Space Antenna,1702.00786. [65]LISA Cosmology Working Groupcollaboration,Cosmology with the Laser Interferometer Space Antenna,Living Rev."},{"citing_arxiv_id":"2604.27376","ref_index":71,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Electroweak Baryogenesis from Collapsing Domain Walls","primary_cat":"hep-ph","submitted_at":"2026-04-30T03:40:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Collapsing axion-like domain walls generate the baryon asymmetry by acting as an effective chemical potential through coupling to the electroweak topological term, with the asymmetry produced via sphaleron processes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Compared to the ordinary EWPT scenario withβ/H∼ O(100), this peak frequency is much lower and the GW signal magnitude is much larger since the \"effective\"β/H takesO(1) value. We plot the observed GW spectrum today in Fig. 4 under three distinct benchmark values as shown in Table I with the expected sensitivity of the future GW observatories. In case I, the GW signal can only be detected by BBO [71] and DECIGO [72]. While in case II without dilution, the GW signal is large enough, falling into the reach window of LISA [73], Taiji [74], Tianqin [75, 76]. Baryon Inhomogeneity-Baryon number is pro- duced only in the regions swept by the domain walls. Consequently, no baryon asymmetry is generated in re- gions that remain inside the 0-domain during the col-"},{"citing_arxiv_id":"2604.20063","ref_index":80,"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":"support","context_text":"persists in the so-calledasteroid-mass window, spanning approximately 10 −16 M⊙ ≲M≲10 −10 M⊙. Within this mass range, PBHs can potentially account for the entire DM [70-72], and their corresponding SIGW signal naturally falls within the sensitivity band of space-based interferometers such as LISA [73, 74], Taiji [75], TianQin [76, 77], DECIGO [78, 79], and BBO [80, 81]. Therefore, constructing a theoretical framework that explains the current PTA data and predicts GW signatures at higher frequencies, while generating a significant PBH DM population, is of considerable phenomenological interest (see, e.g., Refs. [15, 29, 38, 82-118] for related works). However, this interplay between the SIGW amplitude and the PBH abundance also introduces a severe theoretical"},{"citing_arxiv_id":"2604.19197","ref_index":15,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"CP-violating multi-field phase transitions and gravitational waves in a hidden NJL sector","primary_cat":"hep-ph","submitted_at":"2026-04-21T08:07:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Multi-field tunneling analysis in a CP-violating NJL model yields a slow transition (β/H ~ 100) whose stochastic gravitational-wave signal is detectable by μAres and insensitive to the CP angle.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[10] P. A. Seoane et al. (LISA), Living Rev. Rel.26, 2 (2023), 2203.06016. [11] M. Colpi et al. (LISA) (2024), 2402.07571. [12] W.-R. Hu and Y.-L. Wu, Natl. Sci. Rev.4, 685 (2017). [13] J. 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Rev.124, 246 (1961)."},{"citing_arxiv_id":"2604.17478","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Unified Bogoliubov Approach to Primordial Gravitational Waves: From Inflation to Reheating","primary_cat":"hep-ph","submitted_at":"2026-04-19T15:09:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An improved Bogoliubov numerical method computes the full primordial GW spectrum from inflation to reheating and shows that inflaton anharmonicity imprints distinctive features at high frequencies.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"spanning an extraordinarily broad range of frequencies-see Ref. [1] for a comprehensive review. The broad GW spectrum, together with many relevant experimental probes, is schematically illustrated in Fig. 1, where the spectrum extends from ultra-low frequen- cies accessible indirectly via cosmic microwave background (CMB) observations including Planck [2] and future missions like LiteBIRD [3], through the nano-Hz regime targeted by pulsar timing arrays (PTAs) including NANOGrav [4] and SKA [5], up to the Hz band relevant for space-based interferometers such as LISA [6], BBO [7-9], and DECIGO [10]. At even higher frequencies, above MHz or GHz, there has been growing interest in novel detection ideas [11-21] aimed at probing this regime-see Refs."},{"citing_arxiv_id":"2604.14099","ref_index":117,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Electro-Weak Phase Transitions and Collider Signals in the Aligned 2-Higgs Doublet Model","primary_cat":"hep-ph","submitted_at":"2026-04-15T17:14:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The Aligned 2HDM supports strong first-order electroweak phase transitions that yield LISA-detectable gravitational waves together with LHC-accessible signals from additional neutral and charged Higgs states.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Panico,Collision integrals for cosmological phase transitions,JHEP05(2023) 194 [2303.05846]. [115] S. De Curtis, L. Delle Rose, A. 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Shaded regions indicate the sensitivities of current and future detectors, including muAres [67], LISA [68, 69], Taiji [70, 71], TianQin [72], DE- CIGO [73-75], BBO [76, 77] and LIGO-Virgo [78-81], CE [82], and ET [83-85]. corresponding toF a ∈[1.9×10 10,1.4×10 11] GeV. Using Eq. (8) and adopting the conventionf 1 ≤f 2, one obtains Fa < f1 ≤F a p n2 +m 2 ≤f 2.(19) Higher-dimensional operators in Eq. 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