Pith. sign in

REVIEW 2 major objections 5 minor 17 cited by

Higgs-like inflation under ACTivated mass

T0 review · 2 major / 5 minor · reviewed 2026-08-16 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read The paper shows that a positive mass term in the Jordan-frame Higgs potential raises the spectral index of metric Higgs-like inflation into the region preferred by the newest CMB and BAO data.

desk verdict A clean minimal deformation of metric Higgs inflation that raises ns and fits ACT, but the horizon-exit scale sits close to the strong-coupling region and needs a UV-control check before the compatibility claim is solid. read the letter →

arxiv 2505.03004 v1 pith:RMBW2IAC submitted 2025-05-05 hep-ph astro-ph.COgr-qc

Wen Yin This is my paper · ORCID
classification hep-phastro-ph.COgr-qc
keywords metricHiggsinflationJordan-framemasstermspectralindexnon-minimalcouplingslow-rollapproximationtensor-to-scalarratiothresholdcorrectionsquarticpotential
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper aims to show that metric Higgs-like inflation can still fit the latest combined cosmic microwave background and baryon-acoustic-oscillation data if the Jordan-frame potential gains a positive quadratic mass term. The shift matters because the conventional quartic Higgs-inflation and Starobinsky predictions sit below the preferred spectral index. By expanding the Einstein-frame potential, the paper identifies a mild-tuning parameter whose 10 percent adjustment raises the spectral index into the observed region for about 55 to 60 e-folds. It also argues that a mass of the required size can arise from threshold corrections in the Higgs sector, so the fix is not a bare addition.

What carries the argument

The load-bearing object is the expanded Einstein-frame potential $V(h)\simeq \lambda/\xi^2-2\lambda\delta\,\xi^{-3}h^{-2}+(4\delta-1)\lambda\xi^{-4}h^{-4}$, with $\delta=1-m^2\xi/(2\lambda)$. The $h^{-2}$ term is the usual massless Higgs-inflation plateau; the mass term changes its coefficient, and when $\delta$ is of order 0.1, the $h^{-4}$ term becomes sizeable and bends the plateau so that $n_s$ increases. The slow-roll equations then turn this shape change into the observables $N$, $n_s$, and $r$. A one-loop effective-action calculation is used to argue that threshold effects can generate an $m^2$ of the required sign and magnitude.

What would settle it

A direct calculation of the threshold corrections at $h\sim 1/\sqrt{\xi}$ would settle the claim: if those corrections shift $N$ by more than a few tenths, the predicted $n_s$ moves out of the observed band. Alternatively, a measurement of $n_s$ below about 0.970 with 1$\sigma$ precision at the pivot scale would rule out the parameter region the paper highlights.

Watch

Extended reading notes

Core claim

The central discovery is that in metric Higgs(-like) inflation with $V_{\rm JF}=m^2 h^2+\lambda h^4$ and $\xi\gg 1$, the usual attractor predictions are not robust against a quadratic Jordan-frame mass. Expanding the Einstein-frame potential for $h\gg 1/\sqrt{\xi}$ gives $V\simeq \lambda/\xi^2-(2\lambda/\xi^3-m^2/\xi^2)h^{-2}+\cdots$, so the mass term enters the same large-field coefficient that shapes the plateau. Defining $\delta=1-m^2\xi/(2\lambda)$, a mild cancellation makes the $O(h^{-4})$ term important; this accelerates the roll and, for fixed $N$, moves the field to larger $\phi_*$, where the curvature $|\eta_*|$ is smaller, so $n_s$ rises while $r$ remains near the usual small value. The paper demonstrates the effect with a numerical solution of the full equation of motion, showing that a mild 10 percent tuning places the predictions inside the observed 1 to 2$\sigma$ region for $N\approx 55$ to $70$.

Load-bearing premise

The calculation assumes that the slow-roll predictions are valid even though inflation ends near $h\sim 1/\sqrt{\xi}$, where the theory becomes strongly coupled, and that non-perturbative corrections change the e-folding number by at most about 0.1% as asserted in the paper without derivation.

Editorial extensions

If this is right

  • Metric Higgs-like inflation remains a viable explanation of the data; $n_s\simeq 1-2/N$ is not the only prediction this framework can produce.
  • For fixed $N$, a larger quadratic mass (smaller $\delta$) raises $n_s$, and $N\approx 55$ to $60$ with a mild tuning covers the measured central value.
  • The required mass lies between $1/\xi$ and $1/\sqrt{\xi}$ in reduced Planck units for $\xi\lesssim 10^5$, consistent with treating the mass as a soft breaking of scale invariance.
  • The tensor-to-scalar ratio stays below the current upper bound and close to the standard Higgs-inflation value, so the model preserves the attractive small-$r$ prediction.
  • The running of the spectral index is predicted to be small and negative, at the level of $10^{-4}$ and $10^{-5}$, which future data can check.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • I infer that the same mechanism should work in any attractor model where a suppressed operator enters the first post-flat correction of the Einstein-frame potential; scanning such operators would give a one-parameter family of viable $n_s$ values.
  • I infer that a future measurement of $n_s$ with precision near 0.001 will separate this branch from the pure quartic and Starobinsky branches, since they differ by roughly 0.01.
  • I infer that computing the threshold corrections between the strong-coupling scales $1/\xi$ and $1/\sqrt{\xi}$ in a concrete ultraviolet completion would turn the inferred mass parameter into a prediction for the Higgs quartic coupling at inflation energies.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 5 minor

Summary. The paper proposes metric Higgs-like inflation with a Jordan-frame potential V_JF = m^2 h^2 + λ h^4 and a large non-minimal coupling ξ. Defining δ = 1 - m^2 ξ/(2λ), the Einstein-frame potential is expanded for h ≫ 1/√ξ. For δ of order 0.1, the usual O(h^{-2}) term is suppressed and the O(h^{-4}) term accelerates the roll, increasing φ_* for fixed N, which reduces |η_*| and raises n_s. The author solves the full equation of motion numerically (for ξ = 10^3) and finds that a mild tuning of δ lifts n_s into the ACT+BK18+Planck+DESI BAO region for N ≈ 55–60, while keeping r below 0.038. An estimate m ~ 0.0045 (60/N) √(ξ/10^5) is derived from the CMB normalization. Section 3 argues that threshold effects in the UV completion of Higgs inflation can naturally generate the required mass term. The paper concludes that metric Higgs-like inflation is revived by this simple lower-dimensional operator.

Significance. If the central claim holds, the paper offers a minimal, falsifiable resolution of the mild tension between metric Higgs inflation and the recent ACT-based data: a single operator, m^2 h^2, shifts n_s by about 0.005–0.01 while leaving r essentially unchanged. The analytic expansion in Eq. (8) and the δ parametrization are transparent, and the numerical integration of the full equation of motion is a step beyond the slow-roll approximation. The mass-scale estimate in Eq. (14) gives a concrete target for UV completions. The main caveat is that the ACT-fit regime lies close to the strong-coupling scale, so the tree-level predictions require quantitative control of threshold corrections before the compatibility claim is fully established.

major comments (2)
  1. [§2, Fig. 1 and footnote 1] The central numerical prediction is computed at tree level in a regime where the effective field theory is not under control. For the parameters that fit the ACT data (δ ≈ 0.1, N ≈ 60, ξ = 10^3), horizon exit occurs at ξ h_*^2 ≈ 8, i.e. h_* ≈ 3/√ξ, only a factor of about three above the strong-coupling scale 1/√ξ discussed in Sec. 3. The threshold corrections invoked to generate the mass term are expected to be sizable for h up to 1/√ξ and to fall off only for h ≫ 1/√ξ; at ξ h^2 ≈ 8 they can shift the potential by a few percent. Since the mass term itself is only an O(10%) modification of the potential, unquantified UV corrections can shift n_s by an amount comparable to the claimed 0.005–0.01 effect. Footnote 1 only tests sensitivity to the end-of-inflation threshold by varying the condition √(ε^2+η^2)=1/3 between 0.3 and 1, and reports O(0.1%) changes in N; it does not test corrections to the potential at h_*. The statement that 'possible non-perturbative corrections ... modify the estimated N by at most O(0.1%)' is therefore not supported by the numerical check presented.
  2. [§3] The model-building argument for the mass term is qualitative. The one-loop expression in Eq. (15) is presented schematically and is not used to compute the renormalized effective potential or the resulting n_s. The paper does not show that threshold corrections generate the required positive m^2 ≈ 2λ(1-δ)/ξ with δ ≈ 0.1 without simultaneously generating comparable corrections to λ or to higher-dimensional operators that affect n_s at the same order. As a consequence, the claimed compatibility with the ACT data depends on an unspecified portion of the UV completion, and the analysis in Sec. 2 cannot be regarded as a complete prediction of the model.
minor comments (5)
  1. [§2, text before Eq. (11) and footnote 1] The phrase 'When the either two latter term' is ungrammatical; it should be 'When either of the latter two terms dominates'. Also, the typeset 'p ε^2 +η^2' in footnote 1 should read '√(ε^2+η^2)'.
  2. [Eq. (11)] The definition of α is ambiguous: 'If the O(h^{-2})(O(h^{-4})) term dominates, α = 12(3)' should be written as 'α = 12 if the O(h^{-2}) term dominates, and α = 3 if the O(h^{-4}) term dominates.'
  3. [Eq. (14)] The displayed formula is garbled in the typesetting (e.g., 'r ξ 105 60 N'). Please render it cleanly as m ≈ 0.0045 (Δ_R^2/2.1×10^{-9})^{1/2} (ξ/10^5)^{1/2} (60/N).
  4. [Fig. 1 caption] The caption states 'same color coding' but does not identify which colors correspond to N = 50, 60, 70 in the upper panel. Please define the color scheme explicitly.
  5. [Acknowledgments] The phrase 'ISelective Research Fund' appears to be a typographical error; it should presumably read 'a Selective Research Fund'.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the mass-induced shift in n_s is an independent slow-roll calculation, and the threshold discussion is a plausibility argument rather than a fitted prediction.

full rationale

The central derivation is self-contained. Expanding the Einstein-frame potential, Eqs. (8) and (13) compute n_s and r for a given Jordan-frame mass term, and the result that delta ~ 0.1 raises n_s is a genuine dynamical consequence, not an identity built into the definition of delta. Eq. (14) fixes the mass scale from the CMB amplitude and delta ~ 0; this is parameter normalization, not an in-sample fit to n_s. The paper scans delta and compares with ACT/BK18/Planck/DESI contours, which is model parameter estimation rather than a renamed prediction. Threshold effects in Sec. 3 are presented as a possible origin of the mass ('I argue that a mass as large as m ≲ 1/√ξ can arise naturally through threshold effects') and are not used to claim a parameter-free prediction of the exact required m. The author's self-citations ([7,12,16,17,39,46]) appear as supporting references among many external works and are not load-bearing; in particular no uniqueness theorem from prior work is invoked. Footnote 1's assertion that non-perturbative corrections modify N by O(0.1%) is under-supported and a genuine correctness risk, but it is an unquantified error estimate, not a circular reduction of the prediction to its inputs. Therefore the circularity score is 0.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central claim rests on standard slow-roll cosmology, the assumed ACT+BK+Planck+DESI data, the stability of metric Higgs inflation against higher-order operators, and the assertion that non-perturbative effects near h ~ 1/sqrt(xi) are small. The only adjusted parameter is delta, which is tuned to fit ns; xi and N are scanned. No new entities are introduced.

free parameters (3)
  • delta (mass tuning parameter) = scanned in Fig. 1 (0.001 to 0.1); ~0.1 preferred
    delta = 1 - m^2 xi/(2 lambda) controls the mass term. The paper shows a mild 10% tuning (delta ~ 0.1) moves ns into the allowed region. This is the parameter adjusted to fit the observed ns.
  • xi (non-minimal coupling) = 10^3 in numerical study
    Fixed to 10^3 in the numerical example; the author states results are qualitatively independent of xi for xi >> 1. The mass scale estimate depends on xi.
  • N (e-folding number) = 50, 60, 70
    Three values are considered. The preferred fit requires N >= 60, which the paper says can be realized with a short kination epoch.
assumptions (5)
  • domain assumption Slow-roll approximation with a single scalar field and standard Friedmann cosmology
    Used throughout Sec. 2 to compute ns, r from V(phi).
  • domain assumption Combined ACT+BK18+Planck+DESI BAO data give ns = 0.9743 +/- 0.0034 and r < 0.038 (Eq. 1)
    The central motivation; if this data combination is revised, the tension and the paper's significance weaken.
  • domain assumption Metric Higgs inflation is stable against higher-order Planck-suppressed operators (Ref [29])
    Invoked in Sec. 1 and 2 to justify considering only the mass term as the deformation.
  • ad hoc to paper Non-perturbative or threshold effects near h ~ 1/sqrt(xi) modify N by at most O(0.1%) (footnote 1)
    This assumption protects the ns, r predictions from strong-coupling corrections; it is stated but not derived.
  • ad hoc to paper The inflaton can be identified with the SM Higgs at small fields, and threshold corrections at scale between 1/xi and 1/sqrt(xi) generate the required mass (Sec. 3)
    This connects the model to the SM Higgs but requires a UV completion and accepted electroweak fine-tuning.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Higgs-like inflation under ACTivated mass." pith.science (2026). https://pith.science/paper/RMBW2IAC

@misc{pith2026250503004,
  author       = {Pith},
  title        = {Pith review of: Higgs-like inflation under ACTivated mass},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/RMBW2IAC}},
  note         = {Machine review of arXiv:2505.03004}
}
abstract

Recent analyses that combine the latest data from the Atacama Cosmology Telescope (ACT) with cosmic microwave background observations by BICEP/Keck and Planck, together with the DESI baryon acoustic-baryonic-oscillation (BAO) measurements, have tightened the limits on inflationary scenarios. The joint data set yields a spectral index of primordial scalar perturbations $n_s = 0.9743 \pm 0.0034$ and an upper bound on the tensor-to-scalar ratio of $r < 0.038$. This slight upward shift in $n_s$ puts the previously favored Starobinsky model, and the conventional metric Higgs(-like) inflation--based on a quartic potential with a large non-minimal coupling in the Jordan frame--under tension with observations. In metric Higgs-like inflation the attractor behavior makes the predictions remarkably stable against higher-order operators, so modifying $n_s$ through such terms is difficult. In this paper, I show that adding a quadratic mass term to the Jordan-frame potential can raise $n_s$ and restore compatibility with the new data. I also discuss how this mass term can naturally arise from threshold effects in Higgs inflation.

Figures

Figures reproduced from arXiv: 2505.03004 by the authors.

Figure 1
Figure 1. [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 1
Figure 1. Upper panel: spectral index ns versus the tuning parameter δ for N = 50, 60, 70. The purple bands are the ACT + BK18 + Planck + DESI BAO 1 and 2σ regions. Lower panel: corresponding trajectories in the ns-r plane with the same color coding. Hence m ≲ 1/ √ ξ when ξ ≲ 105 (corresponding to λ ≲ 1), while m ≳ 1/ξ when ξ ≳ 103 (i.e. λ ≳ 0.03). Most of parameter region are consistent with the soft breaking assumption impo… view at source ↗

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 17 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. GUT-Scale Smooth Hybrid Inflation with a Stabilized Modulus in Light of ACT and SPT Data

    hep-ph 2025-10 conditional novelty 6.0 of 10

    A smooth hybrid inflation model, augmented with a stabilized modulus, reproduces the spectral index measured by ACT and SPT while keeping Higgs v.e.v.s at the GUT scale.

  2. Kinetically Modified Palatini Inflation Meets ACT Data

    hep-ph 2025-05 conditional novelty 6.0 of 10

    Palatini chaotic inflation with kinetic mixing f_K = f_R^m can shift the predicted spectral index up to the ACT DR6 value n_s = 0.974 while keeping r below current bounds.

  3. Adiabatic Perturbations in GW170817-Compatible Einstein-Gauss-Bonnet Inflation

    gr-qc 2026-08 reject novelty 5.0 of 10

    In Einstein-Gauss-Bonnet inflation, the unconstrained GW170817-compatible models keep perturbations adiabatic, while the constrained class violates adiabaticity in the last few e-foldings.

  4. Induced-Gravity Palatini-Like Higgs Inflation in Supergravity Confronts ACT DR6

    hep-ph 2026-02 unverdicted novelty 5.0 of 10

    A Palatini-supergravity Higgs-inflation model with induced gravity predicts a scalar spectral index ns≈0.972-0.974, consistent with ACT DR6, and favors split supersymmetry with gravitino mass 40-60 PeV.

  5. Fibre Inflation Meets Quintessence: Implications of Perturbative Stabilisation

    hep-th 2025-11 reject novelty 5.0 of 10

    Adding a base-modulus redefinition to fibre inflation in perturbative LVS shifts (ns, r) into ACT-allowed territory and yields an axion quintessence companion.

  6. The BAO-CMB Tension and Implications for Inflation

    astro-ph.CO 2025-07 accept novelty 5.0 of 10

    The upward shift in the scalar spectral index n_s in CMB+BAO analyses is driven by the combined effects of a known CMB degeneracy and the tension between CMB and DESI BAO data, not by new information about n_s itself.

  7. Improved Predictions on Higgs-Starobinsky Inflation and Reheating with ACT DR6 and Primordial Gravitational Waves

    astro-ph.CO 2025-05 conditional novelty 5.0 of 10

    Adding the gravitational-wave bound on extra radiation shrinks the allowed reheating ranges and excludes Higgs-Starobinsky inflation at 1-sigma while leaving a 2-sigma window.

  8. Constraining Quintessential Inflation with ACT: A Gauss-Bonnet Gateway

    astro-ph.CO 2026-04 unverdicted novelty 4.5 of 10

    Exponential and sech Gauss–Bonnet couplings restore ACT-compatible ns and r for quintessential inflation, while tanh fails for a structural sign reason; reheating remains BBN-safe.

  9. Starobinsky Inflation in k-Essence Framework: Attractor Dynamics, Reheating, and Consistency with ACT DR6

    gr-qc 2026-07 conditional novelty 4.0 of 10

    A power-law non-canonical kinetic coupling F(φ)=1+Aφ^n revives the Starobinsky inflation potential's consistency with ACT DR6 CMB data while preserving attractor dynamics and yielding viable reheating.

  10. ACT-DR6 consistent inflation in generalised entropic cosmology and $f(Q)$ gravity

    gr-qc 2026-07 conditional novelty 4.0 of 10

    Reconstruction produces explicit f(Q) and generalised-entropic inflation models (and scalar-coupled versions) whose slow-roll parameters match ACT-DR6 + Planck-BAO constraints on n_s and r.

  11. (Lovelock)$^2$ inflation: explaining the ACT data and equivalence to Higgs-Gauss-Bonnet inflation

    gr-qc 2025-12 conditional novelty 4.0 of 10

    A quadratic f(L) gravity with a negative Gauss-Bonnet coupling shifts Starobinsky inflation's (n_s, r) predictions toward the ACT-preferred higher n_s, at the cost of a larger tensor-to-scalar ratio.

  12. Reconciling Fractional Power Potential and EGB Gravity in the light of ACT

    astro-ph.CO 2025-07 conditional novelty 4.0 of 10

    In EGB gravity, the V0 phi^n potential with n = 1/3 and 2/5 can produce ns and r within the 1 sigma ACT r-ns region for selected coupling values.

  13. What new physics can we extract from inflation using the ACT DR6 and DESI DR2 Observations?

    astro-ph.CO 2025-06 reject novelty 4.0 of 10

    A slow-roll forecast for five non-minimally coupled inflation models in the (ns, αs, βs) plane, claiming future CMB missions will exclude quartic Hilltop and some D-brane scenarios.

  14. GW170817 Viable Einstein-Gauss-Bonnet Inflation Compatible with the Atacama Cosmology Telescope Data

    gr-qc 2025-06 conditional novelty 4.0 of 10

    Einstein-Gauss-Bonnet inflation models with tuned small couplings can reproduce the ACT scalar spectral index and the Planck tensor-to-scalar ratio bound while keeping the gravitational wave speed within the GW170817 limit.

  15. Viability of post-inflationary freeze-in with precision cosmology

    hep-ph 2025-05 conditional novelty 4.0 of 10

    CMB measurements of n_s set a lower bound on the reheating temperature in alpha-attractor inflation, which translates into a strong lower bound on the cut-off scale of a dimension-five UV freeze-in dark matter operator.

  16. Starobinsky like inflation and EGB Gravity in the light of ACT

    astro-ph.CO 2025-05 conditional novelty 4.0 of 10

    Starobinsky inflation with a tuned Einstein-Gauss-Bonnet coupling can reproduce the ACT-enhanced scalar spectral index within 1σ.

  17. Minimal Plateau Inflation in light of ACT DR6 Observations

    astro-ph.CO 2025-05 conditional novelty 3.0 of 10

    A minimal plateau inflation model with exponent n=2 and matter-like reheating remains consistent with the latest CMB datasets at both 1σ and 2σ, while stiffer reheating scenarios are increasingly disfavored.

Reference graph

Works this paper leans on

47 extracted references · 3 canonical work pages · cited by 17 Pith papers

  1. [47]

    Linde, M

    A. Linde, M. Noorbala and A. Westphal, Observational consequences of chaotic inflation with nonminimal coupling to gravity , JCAP 03 (2011) 013 [ 1101.2652]. 12

    arXiv 2011

  2. [1]

    Louis et al., The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and ΛCDM Parameters, 2503.14452

    ACT collaboration, T. Louis et al., The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and ΛCDM Parameters, 2503.14452

    arXiv

  3. [2]

    Calabrese et al., The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models , 2503.14454

    ACT collaboration, E. Calabrese et al., The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models , 2503.14454

    arXiv

  4. [3]

    BICEP, Keck collaboration, P. A. R. Ade et al., Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season , Phys. Rev. Lett. 127 (2021) 151301 [ 2110.00483]

    arXiv 2021

  5. [4]

    Akrami et al., Planck 2018 results

    Planck collaboration, Y. Akrami et al., Planck 2018 results. X. Constraints on inflation, Astron. Astrophys. 641 (2020) A10 [ 1807.06211]

    arXiv 2020

  6. [5]

    Aghanim et al., Planck 2018 results

    Planck collaboration, N. Aghanim et al., Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys. 641 (2020) A6 [ 1807.06209]

    arXiv 2020

  7. [6]

    DESI collaboration, A. G. Adame et al., DESI 2024 VI: cosmological constraints from the measurements of baryon acoustic oscillations , JCAP 02 (2025) 021 [ 2404.03002]

    arXiv 2025

  8. [7]

    Daido, F

    R. Daido, F. Takahashi and W. Yin, The ALP miracle: unified inflaton and dark matter, JCAP 05 (2017) 044 [ 1702.03284]

    arXiv 2017

Show all 47 references
  1. [8]

    Daido, F

    R. Daido, F. Takahashi and W. Yin, The ALP miracle revisited , JHEP 02 (2018) 104 [1710.11107]. 9

    2018 arXiv

  2. [9]

    Czerny and F

    M. Czerny and F. Takahashi, Multi-Natural Inflation, Phys. Lett. B 733 (2014) 241 [1401.5212]

    2014 arXiv

  3. [10]

    Czerny, T

    M. Czerny, T. Higaki and F. Takahashi, Multi-Natural Inflation in Supergravity, JHEP 05 (2014) 144 [ 1403.0410]

    2014 arXiv

  4. [11]

    Takahashi, New inflation in supergravity after Planck and LHC , Phys

    F. Takahashi, New inflation in supergravity after Planck and LHC , Phys. Lett. B 727 (2013) 21 [ 1308.4212]

    2013 arXiv

  5. [12]

    Takahashi and W

    F. Takahashi and W. Yin, Cosmological implications of ns=1 in light of the Hubble tension, Phys. Lett. B 830 (2022) 137143 [ 2112.06710]

    2022 arXiv

  6. [13]

    E. J. Copeland, A. R. Liddle, D. H. Lyth, E. D. Stewart and D. Wands, False vacuum inflation with Einstein gravity , Phys. Rev. D 49 (1994) 6410 [ astro-ph/9401011]

    1994 arXiv

  7. [14]

    G. R. Dvali, Q. Shafi and R. K. Schaefer, Large scale structure and supersymmetric inflation without fine tuning , Phys. Rev. Lett. 73 (1994) 1886 [ hep-ph/9406319]

    1994 arXiv

  8. [15]

    A. D. Linde and A. Riotto, Hybrid inflation in supergravity , Phys. Rev. D 56 (1997) R1841 [hep-ph/9703209]

    1997 arXiv

  9. [16]

    Murase, Y

    K. Murase, Y. Narita and W. Yin, Superheavy dark matter from the natural inflation in light of the highest-energy astroparticle events , 2504.15272

  10. [17]

    Yin, Weak-scale Higgs inflation, JCAP 05 (2024) 060 [ 2210.15680]

    W. Yin, Weak-scale Higgs inflation, JCAP 05 (2024) 060 [ 2210.15680]

    2024 arXiv

  11. [18]

    Jinno, M

    R. Jinno, M. Kubota, K.-y. Oda and S. C. Park, Higgs inflation in metric and Palatini formalisms: Required suppression of higher dimensional operators , JCAP 03 (2020) 063 [1904.05699]

    2020 arXiv

  12. [19]

    I. D. Gialamas and A. B. Lahanas, Reheating in R2 Palatini inflationary models, Phys. Rev. D 101 (2020) 084007 [ 1911.11513]

    2020 arXiv

  13. [20]

    I. D. Gialamas, A. Karam, A. Lykkas and T. D. Pappas, Palatini-Higgs inflation with nonminimal derivative coupling , Phys. Rev. D 102 (2020) 063522 [ 2008.06371]

    2020 arXiv

  14. [21]

    I. D. Gialamas, A. Karam, A. Racioppi and M. Raidal, Has ACT measured radiative corrections to the tree-level Higgs-like inflation? , 2504.06002

  15. [22]

    Dioguardi and A

    C. Dioguardi and A. Karam, Palatini Linear Attractors Are Back in ACTion , 2504.12937

    arXiv

  16. [23]

    Dioguardi, A

    C. Dioguardi, A. J. Iovino and A. Racioppi, Fractional attractors in light of the latest ACT observations, 2504.02809

    arXiv

  17. [24]

    F. L. Bezrukov and M. Shaposhnikov, The Standard Model Higgs boson as the inflaton, Phys. Lett. B 659 (2008) 703 [ 0710.3755]. 10

    2008 arXiv

  18. [25]

    F. L. Bezrukov, A. Magnin and M. Shaposhnikov, Standard Model Higgs boson mass from inflation, Phys. Lett. B 675 (2009) 88 [ 0812.4950]

    2009 arXiv

  19. [26]

    Rubio, Higgs inflation, Front

    J. Rubio, Higgs inflation, Front. Astron. Space Sci. 5 (2019) 50 [ 1807.02376]

    2019 arXiv

  20. [27]

    J. L. Cook, L. M. Krauss, A. J. Long and S. Sabharwal, Is Higgs inflation ruled out? , Phys. Rev. D 89 (2014) 103525 [ 1403.4971]

    2014 arXiv

  21. [28]

    Hamada, H

    Y. Hamada, H. Kawai, K.-y. Oda and S. C. Park, Higgs Inflation is Still Alive after the Results from BICEP2 , Phys. Rev. Lett. 112 (2014) 241301 [ 1403.5043]

    2014 arXiv

  22. [29]

    Bezrukov, J

    F. Bezrukov, J. Rubio and M. Shaposhnikov, Living beyond the edge: Higgs inflation and vacuum metastability , Phys. Rev. D 92 (2015) 083512 [ 1412.3811]

    2015 arXiv

  23. [30]

    Bezrukov and M

    F. Bezrukov and M. Shaposhnikov, Standard Model Higgs boson mass from inflation: Two loop analysis , JHEP 07 (2009) 089 [ 0904.1537]

    2009 arXiv

  24. [31]

    M. He, M. Hong and K. Mukaida, Increase of ns in regularized pole inflation & Einstein-Cartan gravity, 2504.16069

  25. [32]

    Salvio, Independent connection in ACTion during inflation , 2504.10488

    A. Salvio, Independent connection in ACTion during inflation , 2504.10488

    arXiv

  26. [33]

    S. Aoki, H. Otsuka and R. Yanagita, Higgs-Modular Inflation, 2504.01622

    arXiv

  27. [34]

    Kallosh, A

    R. Kallosh, A. Linde and D. Roest, A simple scenario for the last ACT , 2503.21030

    arXiv

  28. [35]

    C. P. Burgess, H. M. Lee and M. Trott, Power-counting and the Validity of the Classical Approximation During Inflation , JHEP 09 (2009) 103 [ 0902.4465]

    2009 arXiv

  29. [36]

    J. L. F. Barbon and J. R. Espinosa, On the Naturalness of Higgs Inflation , Phys. Rev. D 79 (2009) 081302 [ 0903.0355]

    2009 arXiv

  30. [37]

    C. P. Burgess, H. M. Lee and M. Trott, Comment on Higgs Inflation and Naturalness , JHEP 07 (2010) 007 [ 1002.2730]

    2010 arXiv

  31. [38]

    Bezrukov, A

    F. Bezrukov, A. Magnin, M. Shaposhnikov and S. Sibiryakov, Higgs inflation: consistency and generalisations, JHEP 01 (2011) 016 [ 1008.5157]

    2011 arXiv

  32. [39]

    Q. Li, T. Moroi, K. Nakayama and W. Yin, Instability of the electroweak vacuum in Starobinsky inflation, JHEP 09 (2022) 102 [ 2206.05926]

    2022 arXiv

  33. [40]

    D. P. George, S. Mooij and M. Postma, Quantum corrections in Higgs inflation: the Standard Model case, JCAP 04 (2016) 006 [ 1508.04660]

    2016 arXiv

  34. [41]

    Fumagalli and M

    J. Fumagalli and M. Postma, UV (in)sensitivity of Higgs inflation , JHEP 05 (2016) 049 [1602.07234]. 11

    2016 arXiv

  35. [42]

    Enckell, K

    V.-M. Enckell, K. Enqvist and S. Nurmi, Observational signatures of Higgs inflation , JCAP 07 (2016) 047 [ 1603.07572]

    2016 arXiv

  36. [43]

    Bezrukov, M

    F. Bezrukov, M. Pauly and J. Rubio, On the robustness of the primordial power spectrum in renormalized Higgs inflation , JCAP 02 (2018) 040 [ 1706.05007]

    2018 arXiv

  37. [44]

    Shaposhnikov, A

    M. Shaposhnikov, A. Shkerin and S. Zell, Quantum Effects in Palatini Higgs Inflation , JCAP 07 (2020) 064 [ 2002.07105]

    2020 arXiv

  38. [45]

    Poisson, I

    A. Poisson, I. Timiryasov and S. Zell, Critical points in Palatini Higgs inflation with small non-minimal coupling , JHEP 03 (2024) 130 [ 2306.03893]

    2024 arXiv

  39. [46]

    Wada and W

    J. Wada and W. Yin, Gauge coupling jump and small instantons from a large non-minimal coupling, 2411.00768

Pith tools

Reviewed August 16, 2026 · model on record in the stance chip above.