REVIEW 3 major objections 8 minor 46 references
Radiation generates a massive graviton from a continuum gap
Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →
T0 review · glm-5.2
2026-07-09 14:51 UTC pith:X6DIFTOZ
load-bearing objection The one-loop self-energy computation is solid work, but the resonance mass is tuned rather than predicted. the 3 major comments →
Massive Graviton Dark Matter from a Gapped Continuum
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
Core claim
The key finding is that radiative self-energy corrections to a gapped continuum graviton propagator in a linear dilaton background can generate an isolated massive graviton resonance whose mass sits just below the continuum gap, with the dominant contribution to the real part of the self-energy coming from the heaviest brane-localized state, a scalar with mass approximately equal to the five-dimensional Planck scale M_5. When this scalar is identified with the inflaton, its mass around 10^11 GeV triggers a resonance mass near m_g, and the resulting graviton is sufficiently feebly coupled and long-lived to be dark matter. The abundance is set by infrared-dominated freeze-in through QCD散射, not
What carries the argument
The central mechanism is the modification of the brane-to-brane graviton propagator G_h(s) = -1/(m_g + sqrt(m_g^2 - s)) by one-loop self-energy corrections Sigma(s) from brane-localized matter fields. The real part of Sigma, dominated by a heavy scalar of mass m ~ M_5, shifts the propagator denominator and creates a pole at s_p = m_p^2 - i m_p Gamma_p below the continuum threshold m_g, provided Sigma_R = -a*m_g with a in [1,2]. The pole mass is m_p = sqrt(a(2-a))*m_g, the coupling to matter is kappa_chi = sqrt(3(a-1))/M_4, and the width is controlled by the imaginary part of the self-energy from Standard Model states lighter than m_g/2. The holographic fluid arises from the continuum itself,
Load-bearing premise
The existence and location of the isolated graviton resonance requires tuning the five-dimensional Planck mass M_5 relative to the inflaton mass so that the real part of the self-energy satisfies a specific relation to the mass gap. This tuning is imposed by hand rather than derived from an underlying symmetry or dynamical mechanism, meaning the resonance mass is not a prediction but a fitted input.
What would settle it
If the tuning condition Sigma_R = -a*m_g cannot be achieved naturally, or if the one-loop self-energy from Standard Model fields destabilizes the pole location (the condition R << 1 in Eq. 4.16 is violated), the isolated resonance does not exist as a stable dark matter candidate.
If this is right
- If the isolated resonance mechanism is correct, dark matter could be a graviton with mass between roughly 20 keV and 2 MeV, coupled to Standard Model matter through a Wilson coefficient lambda_chi below 0.01, making it effectively invisible to direct detection but potentially testable through improved indirect detection constraints on decaying dark matter.
- The holographic fluid component provides a second dark matter candidate whose abundance scales as T_R^3 * m_g, meaning that measuring or constraining the reheating temperature and the mass gap independently tests the model.
- The brane inflationary model predicts a tensor-to-scalar ratio r ~ 2.7 x 10^{-7} and a spectral index n_s ~ 0.97, which could be tested by future CMB polarization experiments.
- The framework allows two-component dark matter, where the massive graviton and the holographic fluid coexist with abundances summing to the observed value, offering a natural explanation for any future evidence of mixed dark matter components.
Where Pith is reading between the lines
- The tuning condition M_5 = e^{-5/8} m + 4*pi^2*e^{-5/2}*a*m_g + ... (Eq. 4.14) that places the resonance pole at the desired location is not derived from a symmetry or dynamical mechanism, so the resonance mass is effectively a fitted input rather than a prediction unless a stabilization mechanism is identified.
- The claim that physical quantities (pole mass and width) are gauge- and scheme-independent is stated but not explicitly verified, and the one-loop truncation may miss important threshold effects from the continuum itself that could shift or broaden the resonance.
- The infrared-dominated freeze-in through QCD processes at temperatures around the electroweak scale makes the abundance insensitive to the reheating temperature, but this also means the prediction depends on quark masses and the QCD coupling near the confinement transition, introducing hadronic uncertainties.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. This paper studies dark matter candidates in a 5D warped extra-dimensional theory with a linear dilaton background and a gapped continuum graviton spectrum. Two candidates are explored: (1) an isolated massive graviton resonance generated by one-loop self-energy corrections from brane-localized matter (dominated by a heavy scalar/inflaton with mass m ~ M_5), which can be a long-lived FIMP with sub-MeV mass produced via freeze-in; and (2) a holographic fluid arising from the gapped continuum itself, produced via UV freeze-in with abundance controlled by the reheating temperature. The paper also presents a brane inflationary model consistent with recent cosmological observables. The one-loop self-energy calculations in Appendix A, covering scalars, fermions, massive and massless gauge bosons with their Faddeev-Popov ghosts, are detailed and technically careful.
Significance. The paper makes a concrete contribution by computing the full one-loop graviton self-energy in the linear dilaton background across all Standard Model portals, identifying the conditions under which an isolated resonance appears below the continuum gap, and mapping out the viable parameter space for both DM candidates. The connection to unparticle physics (Section 5) and the dual interpretation as a Little String Theory holographic fluid add conceptual depth. The summary plot (Fig. 7) delineating regions where one or both DM components can be present is a useful deliverable. The inflationary model in Section 7, while illustrative, is tied to the DM framework through the inflaton mass requirement m ~ M_5 and yields falsifiable predictions for n_s and r.
major comments (3)
- §4.1, Eqs. (4.3)–(4.14): The existence of the isolated resonance requires the condition Σ_R = -a·m_g with a ∈ [1,2], which demands tuning the 5D Planck mass to M_5 = e^{-5/8}·m + 4π²e^{-5/2}·a·m_g + … . The leading inflaton self-energy scales as m⁴/M_5³ ~ M_5 ~ 10^{10} GeV, while the required value is ~m_g ~ 10^{-3} GeV, implying a tuning precision of ~m_g/M_5 ~ 10^{-14}. The paper is transparent that 'the second one is tuned to find the required solution,' but two issues remain unaddressed: (a) no dynamical mechanism or symmetry is identified that would naturally produce this cancellation, and (b) the stability of the tuning under higher-order corrections is not discussed. A two-loop residual of natural size ~M_5/(16π²)² would overwhelm the required ~m_g unless it also vanishes at the same point M_5 = e^{-5/8}·m. The authors should at minimum comment on whether the vanishing of the one-
- §4.3, Eq. (4.19): The freeze-in yield Ω_χh² ≈ 5.2×10^{-6}·λ_χ²·(GeV/m_χ)³ is adapted from Ref. [23] (Cai, Cacciapaglia, Lee), which studied massive gravitons in a different (RS-like) framework. While the coupling structure κ_χ = λ_χ/M_4 in Eq. (4.11) is analogous to that of Ref. [23], the propagator and resonance structure in the linear dilaton background differ. The paper states the result is 'IR dominated' and 'insensitive to the reheating temperature,' but does not explicitly justify why the LD propagator does not modify the cross-sections for q̄q→gχ and qg→qχ relative to the calculation in Ref. [23]. A brief discussion of what changes (if anything) in the matrix elements due to the gapped continuum propagator would strengthen this central result.
- §4.1, Eq. (4.16) and Fig. 3: The condition ℛ = (3/λ_χ²)·Σ_R^{SM}/m_g ≪ 1 is imposed to ensure that SM contributions (dominated by the top quark, Eq. 4.17) do not disturb the pole location fixed by the inflaton. This condition defines the allowed region in the (λ_χ, m_g) plane, but its dependence on the tuning of M_5 is not fully disentangled. Since M_5 is itself a function of m_g (via Eq. 4.14), the interplay between the inflaton tuning and the SM contribution should be made more explicit — in particular, whether the SM contribution could provide a natural correction that destabilizes or alternatively stabilizes the pole.
minor comments (8)
- §2.2, Eq. (2.38): The notation G_h(z_b, z_b; s) ≡ G_h^-(z_b, z_b; s) - 2m_g/s = G_h^+(z_b, z_b; s) is used throughout, but it would help to state more prominently at first use that the massless graviton pole has been subtracted and that this is the propagator used for all subsequent self-energy calculations.
- §4.1, Eq. (4.6): The Lambert function W is introduced without specifying which branch is used (though the text later says 'principal branch'). A brief note on why the principal branch is the physically relevant one would be helpful.
- §5, Eqs. (5.1)–(5.2): The comparison between D_h = -m_g - √(m_g² - s) and D_un ∝ -(m_g² - s)^{2-d_U} is instructive, but the proportionality constant in D_un is not specified. For the identification d_U = 3/2 to be meaningful, the normalization should be addressed, at least schematically.
- §7.1, Eq. (7.7): The inflationary potential V(ϕ) = V_0 × [(ϕ/μ)² + α(√((ϕ/μ)² + 1) - 1)] is introduced with parameter α < 1, but the role of α in the cosmological predictions (n_s, r) is not explored — only the UV limit is used for the predictions in Eqs. (7.11)–(7.15). It would be useful to state whether the predictions are insensitive to α in the relevant regime, or whether α is fixed by some additional requirement.
- Table 2: The benchmark points use m_g = 1 MeV and m_g = 1 TeV, but the allowed range in Table 1 is 20 keV ≲ m_χ ≲ 2 MeV. The second benchmark point (m_g = 1 TeV) is outside this range and corresponds to the case where the massive graviton decays. This should be stated more explicitly in the text for clarity.
- §6, Eq. (6.7): The supernova bound M_5 ≳ 2.9×10⁵ GeV is noted as 'widely satisfied,' but the lower bound from Table 1 is M_5 ≳ 4×10^{10} GeV. The SN bound is therefore many orders of magnitude weaker and perhaps not worth highlighting unless there are parameter regions where it becomes relevant.
- Fig. 7: The label 'm_g < 20 keV' appears in the lower-left region, but the corresponding exclusion (Lyman-α lower bound) is discussed in §4.4, not in §6 where Fig. 7 is introduced. A cross-reference would help the reader.
- Appendix A: The self-energy results are presented for individual fields, but the total Σ^{SM} used in the main text (Eq. 4.18) sums over the full SM spectrum. It would be useful to provide the explicit numerical value of Σ_R^{SM} (or at least the top contribution, Eq. 4.17) evaluated at a representative benchmark point, to give the reader a sense of the scale.
Circularity Check
No significant circularity; the tuning of M₅ is a naturalness concern, not a definitional loop
full rationale
I walked the full derivation chain and found no step where a claimed prediction reduces to its own inputs by construction. The central calculation—the one-loop self-energy corrections from scalars, fermions, and gauge bosons (Section 3, Appendix A)—is performed from first principles within the paper. The resonance condition Σ_R = −a·m_g (Eq. 4.5) is a standard pole equation; the paper does not define m_p in terms of m_g and then claim to predict m_p from m_g. Instead, it shows that IF the tuning condition on M₅ (Eq. 4.14) is satisfied, THEN a resonance exists with mass m_p = √(a(2−a))·m_g, and the parameter a (or equivalently λ_χ) is scanned over to find the viable DM region. The paper is transparent that Eq. 4.14 involves tuning: 'the second one is tuned to find the required solution.' This is a fine-tuning/naturalness concern, not circularity—the paper does not disguise the tuning as a first-principles prediction. The freeze-in abundance (Eq. 4.19) is taken from Ref. [23] (Cai, Cacciapaglia, Lee—external authors), providing independent support. The holographic fluid framework cites Ref. [17] (overlapping authors), but this is a framework citation: the fluid energy density follows from solving the 5D Einstein equations, which is a legitimate derivation chain, not a self-referential definition. The inflationary model (Section 7) is explicitly presented as illustrative ('for the sake of illustration') and its CMB normalization uses standard formulas. The self-citations to [14–17, 21] establish the model setup but do not constitute a load-bearing circular chain where the central claim reduces to an unverified self-cited ansatz. Score 2 reflects the presence of framework self-citations that are not themselves the target result being derived.
Axiom & Free-Parameter Ledger
free parameters (6)
- m_g (mass gap) =
20 keV - 2 MeV
- a (or lambda_chi) =
a in [1,2], lambda_chi in [0, sqrt(3)]
- m (inflaton mass) =
~8e10 to 4e11 GeV
- T_R (reheating temperature) =
sub-TeV for massive graviton DM
- alpha (inflation potential parameter) =
< 1, unspecified
- mu (inflation potential scale) =
~8.8e-3 * M_5
axioms (6)
- domain assumption The linear dilaton background with bulk potential V(phi) = -3/2 k^2 e^{2phi} is a valid 5D solution dual to Little String Theory.
- domain assumption The brane-to-brane graviton propagator in the absence of a black hole is valid for computing the isolated resonance.
- domain assumption The pole equation D_h(s_p) - Sigma_R(s_p) - i*Sigma_I(s_p) = 0 admits a solution with m_p < m_g in the second Riemann sheet.
- ad hoc to paper The freeze-in yield from Ref. [23] (Cai, Cacciapaglia, Lee) applies to the linear dilaton graviton.
- ad hoc to paper The inflaton is localized on the brane and has mass m ~ M_5.
- domain assumption Standard Model fields are localized on the brane.
invented entities (3)
-
Isolated massive graviton resonance (chi_mu_nu)
independent evidence
-
Holographic fluid
independent evidence
-
Brane-localized inflaton with quadratic-like potential
no independent evidence
read the original abstract
We consider the possibility of dark matter in a warped extra-dimensional theory in presence of a linear dilaton background, with a gapped continuum spectrum, in a brane-world cosmological scenario. Firstly, triggered by self-energy radiative corrections, we study the existence of an isolated resonance of massive gravitons, and its realization as a long-lived feebly interacting dark matter candidate, produced by the freeze-in mechanism. This massive graviton is proved to satisfy all theoretical and experimental constraints, in the sub-MeV mass range. We further consider the close relationship between the existence of this component of dark matter and the presence of an inflaton localized on the brane, with a mass around $10^{11}$ GeV and a sub-TeV reheating temperature, in a brane inflationary scenario that allows to reproduce the most recent cosmological observables. Secondly, the gapped continuum of gravitons, a particular five dimensional realization of the physics of unparticles, is identified as a holographic fluid which can play the role of holographic dark matter. The production of the holographic fluid goes by an ultra-violet freeze-in mechanism, with an abundance mainly depending on the reheating temperature. Depending on the values of the mass gap and the reheating temperature, one or both components of dark matter can be present.
Reference graph
Works this paper leans on
-
[1]
A Large Mass Hierarchy from a Small Extra Dimension
L. Randall and R. Sundrum,A Large mass hierarchy from a small extra dimension,Phys. Rev. Lett.83(1999) 3370–3373, [hep-ph/9905221]
work page internal anchor Pith review Pith/arXiv arXiv 1999
-
[2]
An Alternative to Compactification
L. Randall and R. Sundrum,An Alternative to compactification,Phys. Rev. Lett.83(1999) 4690–4693, [hep-th/9906064]
work page internal anchor Pith review Pith/arXiv arXiv 1999
-
[3]
H. Georgi,Unparticle physics,Phys. Rev. Lett.98(2007) 221601, [hep-ph/0703260]
work page internal anchor Pith review Pith/arXiv arXiv 2007
-
[4]
The Einstein Equations on the 3-Brane World
T. Shiromizu, K.-i. Maeda, and M. Sasaki,The Einstein equation on the 3-brane world, Phys. Rev. D62(2000) 024012, [gr-qc/9910076]
work page internal anchor Pith review Pith/arXiv arXiv 2000
-
[5]
Brane cosmological evolution in a bulk with cosmological constant
P. Binetruy, C. Deffayet, U. Ellwanger, and D. Langlois,Brane cosmological evolution in a bulk with cosmological constant,Phys. Lett. B477(2000) 285–291, [hep-th/9910219]
work page internal anchor Pith review Pith/arXiv arXiv 2000
-
[6]
Randall-Sundrum II Cosmology, AdS/CFT, and the Bulk Black Hole
A. Hebecker and J. March-Russell,Randall-Sundrum II cosmology, AdS / CFT, and the bulk black hole,Nucl. Phys.B608(2001) 375–393, [hep-ph/0103214]
work page internal anchor Pith review Pith/arXiv arXiv 2001
-
[7]
Cosmology of a brane radiating gravitons into the extra dimension
D. Langlois, L. Sorbo, and M. Rodriguez-Martinez,Cosmology of a brane radiating gravitons into the extra dimension,Phys. Rev. Lett.89(2002) 171301, [hep-th/0206146]
work page internal anchor Pith review Pith/arXiv arXiv 2002
-
[8]
Bulk gravitons from a cosmological brane
D. Langlois and L. Sorbo,Bulk gravitons from a cosmological brane,Phys. Rev. D68(2003) 084006, [hep-th/0306281]. 40
work page internal anchor Pith review Pith/arXiv arXiv 2003
-
[9]
Phenomenology of TeV Little String Theory from Holography
I. Antoniadis, A. Arvanitaki, S. Dimopoulos, and A. Giveon,Phenomenology of TeV Little String Theory from Holography,Phys. Rev. Lett.108(2012) 081602, [arXiv:1102.4043]
work page internal anchor Pith review Pith/arXiv arXiv 2012
-
[10]
Radion Dynamics and Phenomenology in the Linear Dilaton Model
P. Cox and T. Gherghetta,Radion Dynamics and Phenomenology in the Linear Dilaton Model,JHEP05(2012) 149, [arXiv:1203.5870]
work page internal anchor Pith review Pith/arXiv arXiv 2012
-
[11]
A brief review of "little string theories"
O. Aharony,A Brief review of ’little string theories’,Class. Quant. Grav.17(2000) 929–938, [hep-th/9911147]
work page internal anchor Pith review Pith/arXiv arXiv 2000
-
[12]
I. Antoniadis, S. Dimopoulos, and A. Giveon,Little string theory at a TeV,JHEP05(2001) 055, [hep-th/0103033]
work page internal anchor Pith review Pith/arXiv arXiv 2001
-
[13]
J. A. Cabrer, G. von Gersdorff, and M. Quir´ os,Soft-Wall Stabilization,New J. Phys.12 (2010) 075012, [arXiv:0907.5361]
work page internal anchor Pith review Pith/arXiv arXiv 2010
-
[14]
Cosmological Dark Matter from a Bulk Black Hole
S. Fichet, E. Meg´ ıas, and M. Quir´ os,Cosmological dark matter from a bulk black hole,Phys. Rev. D107(2023), no. 11 115014, [arXiv:2212.13268]
work page internal anchor Pith review Pith/arXiv arXiv 2023
-
[15]
Holographic Fluids from 5D Dilaton Gravity
S. Fichet, E. Meg´ ıas, and M. Quir´ os,Holographic fluids from 5D dilaton gravity,JHEP08 (2024) 077, [arXiv:2311.14233]
work page internal anchor Pith review Pith/arXiv arXiv 2024
-
[16]
Holography of Linear Dilaton Spacetimes from the Bottom Up
S. Fichet, E. Meg´ ıas, and M. Quir´ os,Holography of linear dilaton spacetimes from the bottom up,Phys. Rev. D109(2024), no. 10 106011, [arXiv:2309.02489]
work page internal anchor Pith review Pith/arXiv arXiv 2024
- [17]
-
[18]
A. Delgado, J. R. Espinosa, J. M. No, and M. Quir´ os,A Note on Unparticle Decays,Phys. Rev. D79(2009) 055011, [arXiv:0812.1170]
work page internal anchor Pith review Pith/arXiv arXiv 2009
-
[19]
E. Meg´ ıas, M. P´ erez-Victoria, and M. Quir´ os,Undecay,JHEP05(2024) 158, [arXiv:2310.16593]
work page internal anchor Pith review Pith/arXiv arXiv 2024
-
[20]
On Continuum Effective Field Theories, Gravity and Holography
S. Fichet, E. Meg´ ıas, and M. Quir´ os,Continuum effective field theories, gravity, and holography,Phys. Rev. D107(2023), no. 9 096016, [arXiv:2208.12273]
work page internal anchor Pith review Pith/arXiv arXiv 2023
-
[21]
E. Meg´ ıas and M. Quir´ os,The Continuum Linear Dilaton,Acta Phys. Polon. B52(2021), no. 6-7 711, [arXiv:2104.10260]
work page internal anchor Pith review Pith/arXiv arXiv 2021
-
[22]
R. K. Mishra, M. Nee, and L. Randall,Inflation with a Growing Fifth Dimension, arXiv:2512.04177
work page internal anchor Pith review Pith/arXiv arXiv
-
[23]
H. Cai, G. Cacciapaglia, and S. J. Lee,Massive Gravitons as Feebly Interacting Dark Matter Candidates,Phys. Rev. Lett.128(2022), no. 8 081806, [arXiv:2107.14548]. [Erratum: Phys.Rev.Lett. 132, 169901 (2024)]
work page internal anchor Pith review Pith/arXiv arXiv 2022
-
[24]
Finite temperature field theory and phase transitions
M. Quir´ os,Finite temperature field theory and phase transitions, inICTP Summer School in High-Energy Physics and Cosmology, pp. 187–259, 1, 1999.hep-ph/9901312
work page internal anchor Pith review Pith/arXiv arXiv 1999
-
[25]
Constraining Light Dark Matter with Diffuse X-Ray and Gamma-Ray Observations
R. Essig, E. Kuflik, S. D. McDermott, T. Volansky, and K. M. Zurek,Constraining Light Dark Matter with Diffuse X-Ray and Gamma-Ray Observations,JHEP11(2013) 193, [arXiv:1309.4091]
work page internal anchor Pith review Pith/arXiv arXiv 2013
-
[26]
Cosmological constraints on exotic injection of electromagnetic energy
V. Poulin, J. Lesgourgues, and P. D. Serpico,Cosmological constraints on exotic injection of electromagnetic energy,JCAP03(2017) 043, [arXiv:1610.10051]
work page internal anchor Pith review Pith/arXiv arXiv 2017
-
[27]
T. R. Slatyer and C.-L. Wu,General Constraints on Dark Matter Decay from the Cosmic Microwave Background,Phys. Rev. D95(2017), no. 2 023010, [arXiv:1610.06933]
work page internal anchor Pith review Pith/arXiv arXiv 2017
-
[28]
21cm signal sensitivity to dark matter decay
G. Facchinetti, L. Lopez-Honorez, Y. Qin, and A. Mesinger,21cm signal sensitivity to dark matter decay,JCAP01(2024) 005, [arXiv:2308.16656]. 41
work page internal anchor Pith review Pith/arXiv arXiv 2024
-
[29]
Y. Sun, J. W. Foster, H. Liu, J. B. Mu˜ noz, and T. R. Slatyer,Inhomogeneous energy injection in the 21-cm power spectrum: Sensitivity to dark matter decay,Phys. Rev. D111 (2025), no. 4 043015, [arXiv:2312.11608]
work page internal anchor Pith review Pith/arXiv arXiv 2025
-
[30]
M. Viel, G. D. Becker, J. S. Bolton, and M. G. Haehnelt,Warm dark matter as a solution to the small scale crisis: New constraints from high redshift Lyman-αforest data,Phys. Rev. D 88(2013) 043502, [arXiv:1306.2314]
work page internal anchor Pith review Pith/arXiv arXiv 2013
-
[31]
M. Viel, G. D. Becker, J. S. Bolton, M. G. Haehnelt, M. Rauch, and W. L. W. Sargent,How cold is cold dark matter? Small scales constraints from the flux power spectrum of the high-redshift Lyman-alpha forest,Phys. Rev. Lett.100(2008) 041304, [arXiv:0709.0131]
work page internal anchor Pith review Pith/arXiv arXiv 2008
-
[32]
F. D’Eramo, A. Lenoci, and A. Dekker,Dark matter freeze-in and small-scale observables: Novel mass bounds and viable particle candidates,Phys. Rev. D112(2025), no. 11 116008, [arXiv:2506.13864]. [33]DESCollaboration, E. O. Nadler et al.,Milky Way Satellite Census. III. Constraints on Dark Matter Properties from Observations of Milky Way Satellite Galaxies...
-
[33]
Unparticle constraints from SN1987A
S. Hannestad, G. Raffelt, and Y. Y. Y. Wong,Unparticle constraints from SN 1987A,Phys. Rev. D76(2007) 121701, [arXiv:0708.1404]
work page internal anchor Pith review Pith/arXiv arXiv 2007
-
[34]
Chaotic inflation on the brane
R. Maartens, D. Wands, B. A. Bassett, and I. Heard,Chaotic inflation on the brane,Phys. Rev. D62(2000) 041301, [hep-ph/9912464]
work page internal anchor Pith review Pith/arXiv arXiv 2000
-
[35]
Braneworld inflation with effective {\alpha}-attractor potential
N. Jaman and K. Myrzakulov,Braneworld inflation with an effectiveα-attractor potential, Phys. Rev. D99(2019), no. 10 103523, [arXiv:1807.07443]. [37]Atacama Cosmology TelescopeCollaboration, T. Louis et al.,The Atacama Cosmology Telescope: DR6 power spectra, likelihoods andΛCDM parameters,JCAP11(2025) 062, [arXiv:2503.14452]. [38]DESICollaboration, M. Abd...
work page internal anchor Pith review Pith/arXiv arXiv 2019
-
[36]
A. Galiautdinov,Logarithmically enhanced hyperbolic square-root deformation of Starobinsky inflation,arXiv:2603.14743
-
[37]
Superconformal generalizations of the Starobinsky model
R. Kallosh and A. Linde,Superconformal generalizations of the Starobinsky model,JCAP06 (2013) 028, [arXiv:1306.3214]
work page internal anchor Pith review Pith/arXiv arXiv 2013
-
[38]
Universality Class in Conformal Inflation
R. Kallosh and A. Linde,Universality Class in Conformal Inflation,JCAP07(2013) 002, [arXiv:1306.5220]
work page internal anchor Pith review Pith/arXiv arXiv 2013
-
[39]
Superconformal Inflationary $\alpha$-Attractors
R. Kallosh, A. Linde, and D. Roest,Superconformal Inflationaryα-Attractors,JHEP11 (2013) 198, [arXiv:1311.0472]
work page internal anchor Pith review Pith/arXiv arXiv 2013
-
[40]
Inflationary Scenarios from Branes at Angles
J. Garcia-Bellido, R. Rabadan, and F. Zamora,Inflationary scenarios from branes at angles, JHEP01(2002) 036, [hep-th/0112147]
work page internal anchor Pith review Pith/arXiv arXiv 2002
-
[41]
Towards Inflation in String Theory
S. Kachru, R. Kallosh, A. D. Linde, J. M. Maldacena, L. P. McAllister, and S. P. Trivedi, Towards inflation in string theory,JCAP10(2003) 013, [hep-th/0308055]
work page internal anchor Pith review Pith/arXiv arXiv 2003
-
[42]
D. H. Lyth,What would we learn by detecting a gravitational wave signal in the cosmic microwave background anisotropy?,Phys. Rev. Lett.78(1997) 1861–1863, [hep-ph/9606387]. 42
work page internal anchor Pith review Pith/arXiv arXiv 1997
-
[43]
A. R. Liddle and S. M. Leach,How long before the end of inflation were observable perturbations produced?,Phys. Rev. D68(2003) 103503, [astro-ph/0305263]. [47]Particle Data GroupCollaboration, S. Navas et al.,Review of particle physics,Phys. Rev. D110(2024), no. 3 030001
work page internal anchor Pith review Pith/arXiv arXiv 2003
-
[44]
First CMB Constraints on the Inflationary Reheating Temperature
J. Martin and C. Ringeval,First CMB Constraints on the Inflationary Reheating Temperature,Phys. Rev. D82(2010) 023511, [arXiv:1004.5525]. [49]PlanckCollaboration, Y. Akrami et al.,Planck 2018 results. X. Constraints on inflation, Astron. Astrophys.641(2020) A10, [arXiv:1807.06211]. [50]SPT-3GCollaboration, E. Camphuis et al.,SPT-3G D1: CMB temperature and...
work page internal anchor Pith review Pith/arXiv arXiv 2010
-
[45]
What does the Bullet Cluster tell us about self-interacting dark matter?
A. Robertson, R. Massey, and V. Eke,What does the Bullet Cluster tell us about self-interacting dark matter?,Mon. Not. Roy. Astron. Soc.465(2017), no. 1 569–587, [arXiv:1605.04307]
work page internal anchor Pith review Pith/arXiv arXiv 2017
-
[46]
S. Y. Choi, J. S. Shim, and H. S. Song,Factorization and polarization in linearized gravity, Phys. Rev. D51(1995) 2751–2769, [hep-th/9411092]. 43
work page internal anchor Pith review Pith/arXiv arXiv 1995
discussion (0)
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