{"total":15,"items":[{"citing_arxiv_id":"2605.21436","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Euclid preparation: Testing multi-field inflation with galaxy power spectrum and bispectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T17:26:36+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Validates redshift-space power spectrum and bispectrum analysis on Abacus-PNG mocks to recover unbiased f_NL constraints for Euclid spectroscopic sample.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"For the same analysis settings as in Sect. 5.4.2, we present addi- tional plots, which complement those shown earlier. Article number, page 27 of 30 A&A proofs:manuscript no. main Table C.1.hoices for priors on cosmological and nuisance parameters. Parameter Prior Cosmology hU [0.6,0.8 ] ωc U[0.085,0.165] 109 ×A s U[1,3.2] fNL U[−500,500] Bias b1 U[0.9,5] b2 U[−20,20] bG2 U[−20,20] bΓ3 U[−20,20] Counter-Term c0 h h−2 Mpc2i N \u0010 0,100 2 \u0011 c2 h h−2 Mpc2i N \u0010 0,100 2 \u0011 c4 h h−2 Mpc2i N \u0010 0,100 2 \u0011 c6 h h−4 Mpc4i N \u0010 0,100 2 \u0011 cB VDG U[−50,50] Shot-Noise s0 N \u0010 0,2 2 \u0011 s02 h h−2 Mpc2i N \u0010 0,10 2 \u0011 s2 h h−2 Mpc2i N \u0010 0,10 2 \u0011 s4 h h−2 Mpc2i N \u0010 0,50 2 \u0011 ˜s1 N \u0010 0,2 2 \u0011 ˜s2 N \u0010 0,2 2 \u0011 ˜s3 N \u0010 0,2 2 \u0011 PNG Counter-Terms"},{"citing_arxiv_id":"2605.20227","ref_index":17,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmological perturbations with $f(R)$ gravity scalarons : Galaxy power spectra and the scalaron mass","primary_cat":"astro-ph.CO","submitted_at":"2026-05-15T08:22:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In a viable f(R) model transitioning from early GR-like to late non-GR behavior, matter power spectra show higher monopole and quadrupole power at small scales with quadrupole elevated at large scales up to k~0.02, while scalaron mass decreases over time to GR limits on galactic scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07720","ref_index":213,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"TopoFisher: Learning Topological Summary Statistics by Maximizing Fisher Information","primary_cat":"stat.ML","submitted_at":"2026-05-08T13:25:25+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"TopoFisher optimizes trainable filtrations, vectorizations, and compressors in persistent homology to maximize Fisher information, yielding higher information than fixed cosmological summaries and approaching neural baselines with far fewer parameters while generalizing better under simulator shifts","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02570","ref_index":89,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Revisiting semiclassical scalar QED in 1+1 dimensions","primary_cat":"hep-th","submitted_at":"2026-05-04T13:21:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Backreaction in semiclassical scalar QED in 1+1D avoids instabilities and produces over-screening at high external charges.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.01619","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Reevaluation of Inflationary Dynamics in Extended General Relativity with Perturbatively and Tensorially Structured Conformal Metric","primary_cat":"gr-qc","submitted_at":"2026-05-02T22:02:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A perturbatively and tensorially structured quantum-deformed conformal metric yields analytical expressions for inflationary observables including quantum corrections to power spectra, spectral indices, and tensor-to-scalar ratio while recovering classical limits.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"4:573, 1987. doi:10.1088/0264-9381/4/3/015. [18] A.H. Guth.The Inflationary Universe: The Quest for a New Theory of Cosmic Origins. Vintage, 1998. ISBN 9780099959502. [19] A.A. Starobinsky. A new type of isotropic cosmological models without singularity.Physics Letters B, 91(1):99-102, 1980. ISSN 0370-2693. doi:https://doi.org/10.1016/0370-2693(80)90670-X. [20] A. Tawfik and E. Abou El Dahab. Flrw cosmology with horava-lifshitz gravity: Impacts of equations of state.International Journal of Theoretical Physics, 56:2122-2139, 2017. doi: https://doi.org/10.1007/s10773-017-3355-1. [21] G. German. Reheating dynamics in inflationary cosmology: insights from attractor and starobinsky models.Eur. Phys. J. Plus, 140, 2025."},{"citing_arxiv_id":"2605.00606","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Non-Supersymmetric Baryogenesis from $U(1)$-Breaking Scalar Dynamics","primary_cat":"gr-qc","submitted_at":"2026-05-01T12:19:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Nonlinear dynamics of a U(1)-breaking complex scalar field generates the observed baryon asymmetry from symmetric initial conditions, with late-time charge density scaling as t^{-3/2} via dynamical freeze-in.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"7 Acknowledgements 20 1 Introduction Thermal history of the Universe after big bang nucleosynthesis (B BN) is well-understood and strongly supported by observations, formin g a key part of the standard cosmological model. This framework faces severa l fundamen- tal challenges, including the horizon, flatness, and monopole proble ms. The idea of inflation [1, 2, 3, 4, 5] provides an elegant solution to these iss ues. However, inflation dilutes any preexisting asymmetry, thus does no t offer an explanation for the observed baryonic abundance in the Universe. It is feasi- ble that baryon-antibaryon asymmetry must generate after the inflationary epoch and it requires physical processes beyond those considere d in standard"},{"citing_arxiv_id":"2604.23224","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Parametric Resonance in $\\phi^4$ Preheating: An Exact Numerical Study","primary_cat":"astro-ph.CO","submitted_at":"2026-04-25T09:31:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Exact numerical simulations of parametric resonance in φ⁴ preheating reveal coupling-dependent behaviors: short-wavelength modes saturate while long-wavelength modes grow gradually in the weak regime, with stochastic and staircase-like production appearing at stronger couplings, differing from prior","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Keywords: Chaotic inflation; Preheating dynamics; Parametric resonance; Numerical analysis. Contents 1 Introduction 2 2 Dynamics of the Inflaton Field 7 3 Dynamics of the created modes 13 4 Numerical Integration 16 5 Discussion and Conclusion 17 ∗hthakur@iitg.ac.in †mknandy@iitg.ac.in(Corresponding Author) 1 arXiv:2604.23224v1 [astro-ph.CO] 25 Apr 2026 1 Introduction The inflationary paradigms of Guth [1], Starobinsky [2], Kazanas [3], and Sato [4] were proposed in the early 80's in order to resolve the flatness, horizon and monopole problems of the standard big-bang cosmology. Subsequently, Linde [5] and Albrecht and Steinhardt [6] proposed the new inflation theory which was further revised by Linde [7] leading to the chaotic inflation theory. Chaotic inflation has been"},{"citing_arxiv_id":"2604.15931","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Robustness of Starobinsky inflation in a minimal two-field scalar-tensor completion","primary_cat":"gr-qc","submitted_at":"2026-04-17T10:43:50+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"On the branch studied here, the entropy mode remains sufficiently suppressed that its sourcing of the curvature perturbation is negligible, while the tensor sector is unchanged. The inflationary observables therefore remain effectively Starobinsky-like, providing a robustness test of Starobinsky inflation against a minimal radiative scalar-tensor deformation. 1 Introduction The Starobinsky model of inflation [1] is one of the best-studied inflationary scenarios. In its simplest form, it predicts a nearly scale-invariant scalar power spectrum and a sufficiently small tensor-to-scalar ratio, both in excellent agreement with thePlanck2018 CMB data [2, 3]. At the same time, recent analyses based on the Atacama Cosmology Telescope (ACT DR6) [4, 5], especially when combined with external datasets, point"},{"citing_arxiv_id":"2604.02823","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Single field slow-roll inflation with step uplift to $n_s=1$","primary_cat":"astro-ph.CO","submitted_at":"2026-04-03T07:41:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"UNKNOWN","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Single-field slow-roll inflation achieves ns=1 by ending inflation suddenly via a large step in the potential.","context_count":1,"top_context_role":"extension","top_context_polarity":"extend","context_text":"990 at least. However, inflation lasts ∆N≈60 does not necessarily requireN ∗,o ≈60 in (1), in particular if the deep slow-roll phase meets a step-like break point of potential so that inflation abruptly ended, see Fig.2. In corresponding scenario, the efolds numberN ∗,o in original popular slow-roll models, such as chaotic inflation [6], Starobinski inflation [4], brane inflation [50-52], can be decom- posed by, using slow-roll approximation, N∗,o ≈ Z ϕ∗,s ϕe,o 1p2εV,o dϕ≡∆N+N o(ϕe,o →ϕ e,s) + ∆Nstep (5) where ∆N= R ϕ∗,s ϕe,s dϕ/p2εV,s ≈60 accounts for the efolds number of slow-roll inflation with the step-modified potential, and No(ϕe,o →ϕ e,s) = Z ϕe,s ϕe,o 1p2εV,o dϕ,(6) corresponds to the efolds number accumulated under the original potential as the inflaton"},{"citing_arxiv_id":"2603.24235","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Non-minimal Effective Scalar-Tensor Gravity in the Early Universe","primary_cat":"gr-qc","submitted_at":"2026-03-25T12:14:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Non-minimal effective scalar-tensor gravity supports early-universe bounce, inflation, and genesis while producing two Hubble values that could resolve the Hubble tension.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.23687","ref_index":42,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Review of strongly coupled regimes in gravity with Dyson-Schwinger approach","primary_cat":"gr-qc","submitted_at":"2026-03-24T19:51:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Dyson-Schwinger methods applied to gravity theories produce conformally flat metrics and a sequence of cosmological phase transitions from conformal symmetry breaking that non-minimal scalar couplings can suppress.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.06521","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Comment on: \"Third-order corrections to the slow-roll expansion: Calculation and constraints with Planck, ACT, SPT, and BICEP/Keck [2025 PDU 47 101813]\"","primary_cat":"astro-ph.CO","submitted_at":"2026-03-06T18:05:19+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Several terms in the third-order slow-roll power spectra are incorrect because three-dimensional integrals were evaluated by integrating a truncated Taylor expansion instead of Taylor-expanding the integral.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.24215","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Neutrino Mass, Vacuum Stability and Higgs Inflation with Vector-Like Quarks and a Single Right-Handed Neutrino","primary_cat":"hep-ph","submitted_at":"2025-12-30T13:26:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The Standard Model extended by n vector-like quarks and one right-handed neutrino stabilizes the Higgs quartic to the Planck scale, produces viable neutrino masses via Type-I seesaw, and yields inflationary observables n_s and r consistent with Planck and ACT data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.21189","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Higgs pole inflation with loop corrections in light of ACT results","primary_cat":"hep-ph","submitted_at":"2025-06-26T12:48:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Loop corrections to the inflaton quartic coupling in pole inflation models shift the spectral index to align with ACT results, with different one-loop and two-loop requirements depending on the sign of the beta function b1.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1807.06211","ref_index":181,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Planck 2018 results. X. Constraints on inflation","primary_cat":"astro-ph.CO","submitted_at":"2018-07-17T04:05:09+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Updated Planck CMB measurements give ns = 0.9649 ± 0.0042, r < 0.056, confirm flatness at 0.4 percent, and show no evidence for scale-dependent features or non-slow-roll dynamics in the inflaton potential.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"29 and 52 months of observations for the high frequency instru- ment (HFI) and low frequency instrument (LFI), respectively. The ideas underlying cosmic inflation were developed dur- ing the late 1970s and early 1980s in order to remedy a number of defects of the hot big-bang cosmological model (e.g., the horizon, smoothness, flatness, and monopole prob- lems) (Brout et al. 1978; Starobinsky 1980; Kazanas 1980; Sato 1981; Guth 1981; Linde 1982; Albrecht & Steinhardt 1982; Linde 1983). Subsequently, it was realized that, on account of quantum vacuum fluctuations, cosmic inflation also provides a means to generate the primordial cosmological perturbations (Mukhanov & Chibisov 1981, 1982; Hawking 1982; Guth & Pi 1982; Starobinsky 1982; Bardeen et al."}],"limit":50,"offset":0}