{"total":11,"items":[{"citing_arxiv_id":"2605.20332","ref_index":82,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the inflationary history of the Universe: semi-simple groups at multi-TeV scales require a low-scale reheating, while independent information on inflation or reheating can directly con- strain the structure of viable flavour completions. In particular, a primordial gravitational- wave signal in CMBB-mode searches, such as LiteBIRD [140-142], CMB-S4 [143-145], Si- mons Observatory [146-148], or BICEP/Keck [82, 84], or in stochastic gravitational-wave searches with pulsar-timing arrays, LISA [92, 93], Einstein Telescope (ET) [94-96], Cosmic Explorer (CE) [97] and intermediate-frequency proposals [98-104], pointing to reheating tem- peratures well aboveO(10 4) TeV, would either exclude semi-simple flavour completions in this range or require highly non-minimal mechanisms capable of efficiently diluting or annihilat-"},{"citing_arxiv_id":"2605.10197","ref_index":42,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Controlled Penumbral Inflation from Monodromic Valleys","primary_cat":"hep-ph","submitted_at":"2026-05-11T08:46:27+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"geometrical upper bound on the inflaton range, JHEP (05), 001, arXiv:1801.05434 [hep-th]. [40] F. Marchesano, D. Prieto, and M. Wiesner, F-theory flux vacua at large complex structure, JHEP (08), 077, arXiv:2105.09326 [hep-th]. [41] Y. Akramiet al.(Planck), Planck 2018 results. X. con- straints on inflation, Astron. Astrophys.641, A10 (2020), arXiv:1807.06211 [astro-ph.CO]. [42] M. Tristramet al.(BICEP/Keck and Planck), Im- proved limits on the tensor-to-scalar ratio using BICEP and Planck data, Phys. Rev. D105, 083524 (2022), arXiv:2112.07961 [astro-ph.CO]. [43] T. Ghignaet al.(LiteBIRD), The LiteBIRD mission to explore cosmic inflation, arXiv e-prints (2024), arXiv:2406.02724 [astro-ph.IM]. [44] K. N. Abazajianet al.(CMB-S4), CMB-S4: Forecasting"},{"citing_arxiv_id":"2605.08931","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"F-Term Hybrid Inflation with T-Model K\\\"ahler Geometry and Beyond","primary_cat":"hep-ph","submitted_at":"2026-05-09T13:05:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"F-term hybrid inflation with SU(1,1)/U(1) or SU(2)/U(1) Kähler geometry in GUTs can be realized without inflationary extrema for broad parameters, matching ACT/SPT data via curvature and tadpole adjustments while predicting cosmic string gravitational waves.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"Shafi for useful discussions and M. Ashry for collaboration during an early stage of this work. References [1] J. Martin, C. Ringeval and V . Vennin,Encyclopædia Inflationaris,Phys. Dark Univ.5, 75 (2014) [arXiv:1303.3787]. [2] Y . Akramiet al.[PlanckCollaboration],Planck 2018 results. X. Constraints on inflation,Astron. Astrophys. 641, A10 (2020) [arXiv:1807.06211]. [3] M. Tristramet al.,Improved limits on the tensor-to-scalar ratio using BICEP and Planck,Phys. Rev. Lett. 127, 151301 (2021) [arXiv:2112.07961]. [4] T. Louiset al.[ACT Collaboration],The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods andΛCDM Parameters,arXiv:2503.14452. [5] E. Calabreseet al.[ACT Collaboration],The Atacama Cosmology Telescope: DR6 Constraints on Extended"},{"citing_arxiv_id":"2605.05295","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Ultraviolet completion of Starobinsky inflation","primary_cat":"hep-th","submitted_at":"2026-05-06T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A supergravity construction using two chiral superfields embeds arbitrary F(R) gravity as a UV completion of Starobinsky inflation, stabilized by the dilaton and consistent with swampland constraints in a heterotic string example.","context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"there are strong theoretical reasons that it should be part of the underlying fundamental theory of gravity , such as string theory , and may play important an role at higher energy scales and particularly in cosmology [1, 2]. In this context, the Starobinsky model of inflation [3], which is very attractive because of its simplicity and very good description of the observational data [4, 5, 6], is known to have a minimal supersymmetric extension as ordinaryN= 1supergravity coupled to two chiral multiplets [7]. One of the two contains the scalar degree of freedom of R2 gravity that plays the role of the inflaton which is complexified due to supersymmetry , and the other contains the goldstino of spontaneously broken supersymmetry during inflation [8, 9]."},{"citing_arxiv_id":"2604.05078","ref_index":61,"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":"Our derivation of the GW spectrum associated with the growth of theχfluctuations assumes that the evolution of the spectator mode function is independent, following the linear system (3.2). In the presence of backreaction and rescatterings, mode-mode couplings induced by the fragmentation of the inflaton field can no longer be ignored, and the Hartree approximation breaks down [61, 96]. The dynamics of the system can still be tracked by means of lattice methods, but analytical control over the computation is lost. In the figure we show as fully opaque curves those computed in the Hartree approximation, and as translucent curves those determined from the lattice. We find that only for couplings close to the backreaction regime are noticeable deviations found."},{"citing_arxiv_id":"2603.15585","ref_index":110,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"QCD-driven dark matter: AQNs formation and observational tests","primary_cat":"hep-ph","submitted_at":"2026-03-16T17:46:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Dark matter is composed of composite quark-antiquark objects stabilized by axion domain walls, offering a unified account of dark matter and baryon asymmetry.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ma ∼ 25-400 µeV. Several key characteristics of the two scenarios are contrasted in Table 8. 5.4.2 Inflationary Hubble scale upper bound The current observational upper bound on HI is derived from limits on the tensor-to-scalar ratio of primordial perturbations, r, measured in the CMB. Current data constrain this ratio to r < 0.032 at 95% confidence [110], which translates into: HI ≃ (1014 GeV) s r 0.01 ≲ 6 × 1013 GeV (32) • In the pre-inflation scenario HI must also be sufficiently small to prevent excessive axion isocurvature fluctuations δa ∼ HI 2π. In this case, CMB observations lead to a much tighter upper bound on HI: HI ≲ (1.6 × 107 GeV) θi 10 µeV ma ‹ ΩDM Ωa . (33) Assuming ΩDM = Ωa, this does not lead to an observational conflict with (Eq."},{"citing_arxiv_id":"2603.11026","ref_index":8,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Blind mitigation of foreground-induced biases on primordial $B$ modes for ground-based CMB experiments","primary_cat":"astro-ph.CO","submitted_at":"2026-03-11T17:50:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Two NILC extensions—one deprojecting foreground moments and one marginalizing residuals at the likelihood level—yield unbiased r estimates and consistent lensing B-mode reconstruction in SO-SAT-like simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.25013","ref_index":69,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational waves from axion inflation in the gradient expansion formalism. Part II. Fermionic axion inflation","primary_cat":"astro-ph.CO","submitted_at":"2025-09-29T16:38:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Schwinger fermion production in axion inflation damps gauge fields, enabling observable primordial gravitational waves in LISA/ET bands while satisfying ΔN_eff limits and identifying a new damped-oscillation backreaction regime.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.00798","ref_index":107,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational waves from axion inflation in the gradient expansion formalism. Part I. Pure axion inflation","primary_cat":"astro-ph.CO","submitted_at":"2025-08-01T17:24:57+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"In pure axion inflation, detectable gravitational wave signals arise only in parameter regions with strong backreaction that violate the upper bound on ΔN_eff.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.10534","ref_index":15,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"ACT-ing on inflation: Implications of non Bunch-Davies initial condition and reheating on single-field slow roll models","primary_cat":"astro-ph.CO","submitted_at":"2025-05-15T17:45:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Non-Bunch-Davies initial conditions substantially improve the fit of various single-field slow-roll inflation models to updated n_s-r constraints from ACT DR6 combined with Planck, DESI, and BICEP/Keck data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"an additional degree of freedom and enlarges the allowed parameter space forn S. We therefore report the bounds on nS for r = 0. At this point, we should also mention that the value of nS = 0.9743 ± 0.0034 that we have used in this work was obtained by taking into account the result of DESI DR1, which assumes ΛCDM [ 8, 9]. On the other hand, the result of DESI DR2 [ 15], strongly disfavors ΛCDM. Hence, to consider DESI DR2 results, it is advisable to wait for the more recent data release by DESI (for a detailed discussion on this, see [15, 16]). In [17], the authors varied, in addition to the six stan- dard cosmological parameters, extra parameters such as the running of the scalar spectral index, the tensor-to-"},{"citing_arxiv_id":"2501.06451","ref_index":48,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"On Legacy of Starobinsky Inflation","primary_cat":"gr-qc","submitted_at":"2025-01-11T06:48:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A memorial review of the Starobinsky inflation model that proposes a deformation for primordial black hole production and discusses superstring quantum corrections plus universal reheating.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}