{"total":16,"items":[{"citing_arxiv_id":"2606.29796","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Superhorizon curvature perturbations in hybrid inflation revisited","primary_cat":"astro-ph.CO","submitted_at":"2026-06-29T05:15:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Hybrid inflation produces enhanced curvature perturbations with a broad power spectrum peak featuring k^3 infrared growth and positive f_NL fixed by tachyonic waterfall geometry, potentially accounting for PBH dark matter and LISA-detectable SGWB.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24868","ref_index":260,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Exploring Gravitational Wave Signatures Due to Primordial Non-gaussianity and Large Scale Structure Using SKAO","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T17:47:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Explores SKAO detection of scalar-induced GW backgrounds as probes of primordial non-Gaussianity and parity violation, with LSS cross-correlation to improve SNR.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00176","ref_index":55,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Eigenvalue formulation of Stochastic Inflation and application to large perturbation generating inflationary features","primary_cat":"astro-ph.CO","submitted_at":"2026-05-29T13:57:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A new eigenvalue method is introduced to compute the PDF of stochastic e-folds in inflation, recovering a known flat-potential result and analyzing constant-drift cases in narrow and broad well limits.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14044","ref_index":70,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Magnetic Origin of Primordial Black Holes: Ultralight PBHs and Secondary GWs","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T19:06:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Inflationary magnetic fields induce curvature perturbations that form ultralight PBHs, generating a stochastic GW background with model-specific features.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Astrophys.641, A10 (2020), arXiv:1807.06211 [astro-ph.CO]. [67] T. M. C. Abbottet al.(DES), Phys. Rev. D105, 023520 (2022), arXiv:2105.13549 [astro-ph.CO]. [68] J. Garcia-Bellido and E. Ruiz Morales, Phys. Dark Univ.18, 47 (2017), arXiv:1702.03901 [astro-ph.CO]. [69] H. Motohashi and W. Hu, Phys. Rev. D96, 063503 (2017), arXiv:1706.06784 [astro-ph.CO]. [70] C. T. Byrnes, P. S. Cole, and S. P. Patil, JCAP06, 028 (2019), arXiv:1811.11158 [astro-ph.CO]. [71] G. Ballesteros, J. Beltran Jimenez, and M. Pieroni, JCAP06, 016 (2019), arXiv:1811.03065 [astro-ph.CO]. [72] R. N. Raveendran, K. Parattu, and L. Sriramkumar, Gen. Rel. Grav.54, 91 (2022), arXiv:2206.05760 [astro-ph.CO]. [73] H. V. Ragavendra, P. Saha, L."},{"citing_arxiv_id":"2605.13325","ref_index":24,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Fixing the Renormalization of Inflationary Loops via Ward Identities","primary_cat":"gr-qc","submitted_at":"2026-05-13T10:39:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Ward identities from large gauge symmetry impose model-independent constraints on renormalizing inflationary loops and non-perturbatively govern the infrared power spectrum evolution.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"Astro- phys.678, A50 (2023), arXiv:2306.16214 [astro-ph.HE]. [21] J. Antoniadiset al.(EPTA), Astron. Astrophys.678, A48 (2023), arXiv:2306.16224 [astro-ph.HE]. [22] H. Xuet al., Res. Astron. Astrophys.23, 075024 (2023), arXiv:2306.16216 [astro-ph.HE]. [23] M. H. Namjoo, H. Firouzjahi, and M. Sasaki, EPL101, 39001 (2013), arXiv:1210.3692 [astro-ph.CO]. [24] J. Garcia-Bellido and E. Ruiz Morales, Phys. Dark Univ.18, 47 (2017), arXiv:1702.03901 [astro-ph.CO]. [25] C. Germani and T. Prokopec, Phys. Dark Univ.18, 6 (2017), arXiv:1706.04226 [astro-ph.CO]. [26] H. Motohashi and W. Hu, Phys. Rev. D96, 063503 (2017), arXiv:1706.06784 [astro-ph.CO]. [27] W.-T. Xu, J. Liu, T.-J. Gao, and Z.-K. Guo, Phys. Rev."},{"citing_arxiv_id":"2605.11956","ref_index":43,"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":"unclear","context_text":"04466 [hep-ph]. [40] J. J. Bennett, G. Buldgen, P. F. De Salas, M. Drewes, S. Gariazzo, S. Pastor, and Y. Y. Y. Wong, JCAP04, 073 (2021), arXiv:2012.02726 [hep-ph]. [41] M. Escudero, G. Jackson, M. Laine, and S. Sandner, JCAP02, 046 (2026), arXiv:2511.04747 [hep-ph]. [42] N. Barnaby and Z. Huang, Phys. Rev. D80, 126018 (2009), arXiv:0909.0751 [astro-ph.CO]. [43] J. Garcia-Bellido and E. Ruiz Morales, Phys. Dark Univ.18, 47 (2017), arXiv:1702.03901 [astro-ph.CO]. [44] G. Ballesteros, M. A. G. Garc' ıa, A. P. Rodr' ıguez, M. Pierre, and J. Rey, JCAP12, 006 (2022), arXiv:2208.14978 [astro-ph.CO]. [45] O. ¨Ozsoy and G. Tasinato, Universe9, 203 (2023), arXiv:2301.03600 [astro-ph.CO]. [46] H. Wang, Y.-l. Zhang, and T."},{"citing_arxiv_id":"2605.08336","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Primordial Black Hole Hotspots Beyond Flat Spacetime","primary_cat":"hep-ph","submitted_at":"2026-05-08T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Hotspots around light primordial black holes cool faster in an expanding universe following T_plt ∝ t^{-11/15} and vanish completely in finite time, unlike everlasting hotspots in flat spacetime.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Zel'dovich and I. D. Novikov, Sov. Astron.10, 602 (1967). [2] B. J. Carr and S. W. Hawking, Mon. Not. Roy. Astron. Soc.168, 399 (1974). [3] B. J. Carr, Astrophys. J.201, 1 (1975). [4] J. Yokoyama, Astron. Astrophys.318, 673 (1997), arXiv:astro-ph/9509027. [5] J. Garcia-Bellido, A. D. Linde, and D. Wands, Phys. Rev. D54, 6040 (1996), arXiv:astro-ph/9605094. [6] J. Garcia-Bellido and E. Ruiz Morales, Phys. Dark Univ. 18, 47 (2017), arXiv:1702.03901 [astro-ph.CO]. [7] S. W. Hawking, I. G. Moss, and J. M. Stewart, Phys. Rev. D26, 2681 (1982). [8] I. G. Moss, Phys. Rev. D50, 676 (1994). [9] M. Y. Khlopov, R. V. Konoplich, S. G. Rubin, and A. S. Sakharov, (1998), arXiv:hep-ph/9807343. [10] T. H. Jung and T. Okui, (2021), arXiv:2110."},{"citing_arxiv_id":"2604.06858","ref_index":10,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Memory-Burden Suppression of Hawking Radiation and Neutrino Constraints on Primordial Black Holes","primary_cat":"hep-ph","submitted_at":"2026-04-08T09:20:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Memory-burden backreaction deforms the Hawking spectrum to suppress its high-energy tail, lowering total luminosity and neutrino flux by a factor set by a single suppression parameter and thereby relaxing IceCube bounds on primordial black hole dark matter.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Polnarev and R. Zembowicz, Phys. Rev. D43, 1106 (1991). [6] M. Crawford and D. N. Schramm, Nature298, 538 (1982). [7] S. W. Hawking, I. G. Moss, and J. M. Stewart, Phys. Rev. D26, 2681 (1982). [8] H. Kodama, M. Sasaki, and K. Sato, Prog. Theor. Phys.68, 1979 (1982). [9] J. Garcia-Bellido and E. Ruiz Morales, Phys. Dark Univ.18, 47 (2017), 1702.03901. [10] J. S. Bullock and J. R. Primack, Phys. Rev. D55, 7423 (1997), astro-ph/9611106. [11] P. Ivanov, P. Naselsky, and I. Novikov, Phys. Rev. D50, 7173 (1994). [12] S. M. Leach, I. J. Grivell, and A. R. Liddle, Phys. Rev. D62, 043516 (2000), astro-ph/0004296. [13] C. T. Byrnes, P. S. Cole, and S. P. Patil, JCAP06, 028 (2019), 1811.11158. [14] G. Ballesteros and M."},{"citing_arxiv_id":"2602.07972","ref_index":93,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Self-resonance preheating in deformed attractor models: oscillon formation and evolution","primary_cat":"astro-ph.CO","submitted_at":"2026-02-08T13:51:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Deformed alpha-attractor T-models with a Gaussian feature near the minimum yield more smaller shorter-lived oscillons during self-resonance preheating, suppressing energy in oscillons and altering the high-frequency gravitational wave tail while leaving low frequencies unchanged.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"Phys. Lett. B776, 345 (2018), arXiv:1705.04861 [astro- ph.CO]. [90] H. Motohashi and W. Hu, Phys. Rev. D96, 063503 (2017), arXiv:1706.06784 [astro-ph.CO]. [91] K. Kannike, L. Marzola, M. Raidal, and H. Veerm¨ ae, JCAP09, 020, arXiv:1705.06225 [astro-ph.CO]. [92] G. Ballesteros and M. Taoso, Phys. Rev. D97, 023501 (2018), arXiv:1709.05565 [hep-ph]. [93] O. ¨Ozsoy, S. Parameswaran, G. Tasinato, and I. Zavala, JCAP07, 005, arXiv:1803.07626 [hep-th]. [94] M. Cicoli, V. A. Diaz, and F. G. Pedro, JCAP06, 034, arXiv:1803.02837 [hep-th]. [95] S. S. Mishra and V. Sahni, JCAP04, 007, arXiv:1911.00057 [gr-qc]. [96] K. Inomata, E. McDonough, and W. Hu, Phys. Rev. D 104, 123553 (2021), arXiv:2104.03972 [astro-ph."},{"citing_arxiv_id":"2508.10812","ref_index":14,"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":"2506.21423","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Towards Stochastic Inflation in Higher-Curvature Gravity","primary_cat":"gr-qc","submitted_at":"2025-06-26T16:07:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Stochastic inflation with Gauss-Bonnet coupling to the inflaton yields first-passage-time estimates of the scalar power spectrum and PBH mass fraction in slow-roll and ultra-slow-roll limits.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2502.10287","ref_index":73,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hamiltonians to all Orders in Perturbation Theory and Higher Loop Corrections in Single Field Inflation with PBHs Formation","primary_cat":"astro-ph.CO","submitted_at":"2025-02-14T16:50:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Derives all-order Hamiltonians via EFT of inflation for USR models and shows L-loop corrections to CMB-scale perturbations scale as (ΔN P_e L)^L, exiting perturbative control at L=4 for typical ΔN≈2.5.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2502.09481","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Non-Perturbative Hamiltonian and Higher Loop Corrections in USR Inflation","primary_cat":"astro-ph.CO","submitted_at":"2025-02-13T16:44:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"In USR inflation with an idealized instantaneous sharp transition to slow-roll, higher loop corrections to curvature perturbations on CMB scales grow rapidly with loop order L and may exit perturbative control.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2109.01398","ref_index":252,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2006.02838","ref_index":289,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primordial Black Holes as Dark Matter: Recent Developments","primary_cat":"astro-ph.CO","submitted_at":"2020-06-03T17:57:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Primordial black holes in specific mass ranges could account for some or all dark matter while resolving structure-formation and seed problems in standard cosmology.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"There are many inflationary models and they predict a variety of shapes for δrms(M). Some of them produce an extended plateau or dome-like feature in the power spectrum. For example, this applies for two-field models like hybrid inflation [29] and even some single-field models like Higgs inflation [287, 288], although this may not apply for the minimal Higgs model [289]. Instead of focussing on any specific scenario, Reference [74] assumes a quasi-scale-invariant spectrum, δrms(M) = A ( M M⊙ )(1−ns)/4 , (V.4) where the spectral index ns and amplitude A are treated as free phenomenological parameters. This could 24 Primordial Black Holes as Dark Matter: Recent Developments �� -� �� -� ���� �� �� � �� � �� -� �����"},{"citing_arxiv_id":"2002.12778","ref_index":57,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on Primordial Black Holes","primary_cat":"astro-ph.CO","submitted_at":"2020-02-27T05:17:54+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Updated compilation shows PBHs are tightly constrained across 55 orders of magnitude in mass, ruling out dominant dark matter contributions except in narrow windows, with many limits carrying observational uncertainties.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"so this was a feature of an early model of PBH production [53]. Similar models were subsequently studied for a polynomial potential with [54] or without [55] a logarithmic correction, a non-minimally coupled scalar field with a quartic potential [56] and a quintic potential fine-tuned so that a local minimum is followed by a small maximum (so that the field is slowed down but can still exit this region) [57]. Ultra-slow roll inflation occurs in the limit of a flat potential [58] and curvature perturbations then grow rapidly on superhorizon scales, rather than remaining constant, so the standard expression for the power spectrum is not valid and a more precise numerical calculation is required [59]. Rapid growth of superhorizon fluctuation is not limited to the case of ultra-slow roll, as it also"}],"limit":50,"offset":0}