arxiv: 2605.04166 · v1 · submitted 2026-05-05 · ✦ hep-ph

Recognition: 3 theorem links

· Lean Theorem

Long Inflation Screens Euclidean-Wormhole Initial States

Imtiaz Khan , Pirzada , G. Mustafa , Farruh Atamurotov , Chengxun Yuan

Authors on Pith no claims yet

Pith reviewed 2026-05-08 17:46 UTC · model grok-4.3

classification ✦ hep-ph

keywords Euclidean wormholesinflationary initial conditionsBunch-Davies vacuumBogoliubov coefficientscosmic microwave backgroundprimordial perturbations

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The pith

Long inflation erases detectable traces of Euclidean wormhole initial states from the cosmic microwave background.

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

Euclidean wormholes can set up the early universe in non-standard initial conditions before inflation starts. The paper demonstrates that sufficiently long expansion afterward screens these conditions so thoroughly that the resulting perturbations match the standard Bunch-Davies vacuum on observable scales. A visibility bound shows the deviation amplitude falls exponentially with the number of pre-observable e-folds, while any leftover effects are pushed to a specific comoving scale tied to the wormhole. Only if inflation lasted close to its minimum duration, or if that special scale falls inside our current window, would scalar, tensor, or higher-order imprints remain visible. This converts the absence of such imprints into a direct limit on how long inflation must have lasted.

Core claim

Euclidean wormholes can prepare inflation in non-Bunch-Davies initial states, but long Lorentzian expansion screens this memory from the CMB. We derive a visibility bound for Euclidean-matched Bogoliubov data: the pivot excitation satisfies |β_*| ≲ e^{-2N_pre}, and smooth Euclidean filters confine residual signatures to a comoving edge k_w = a_i M. Only near-minimal inflation, or an edge inside the observable window, leaves detectable scalar, tensor, and higher-point imprints. For longer inflation, wormhole-prepared perturbations are driven to the Bunch-Davies prediction. Euclidean memory therefore becomes a quantitative bound on inflationary duration, with direct targets in CMB polarization

What carries the argument

The visibility bound on the Bogoliubov coefficient β_* measuring deviation from the Bunch-Davies vacuum, exponentially suppressed by the number of pre-inflation e-folds.

If this is right

Detectable imprints from wormhole initial states require inflation to be near its minimum duration.
Any residual signatures are confined to one specific comoving scale set by the wormhole radius.
These imprints would appear in scalar and tensor power spectra as well as higher-order correlations.
The lack of such features in current data supplies a lower bound on the total length of inflation.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

Future CMB polarization measurements at large angular scales offer a direct test of whether any wormhole-scale edge falls inside the observable window.
The same screening logic could apply to other proposed non-standard initial conditions, turning their absence into a duration constraint.
Large-scale structure surveys could search for the predicted scale-dependent deviations if the wormhole edge lies near the horizon scale today.

Load-bearing premise

Euclidean wormholes prepare specific non-Bunch-Davies initial states that can be matched via Bogoliubov coefficients to Lorentzian inflation, with smooth filters confining signatures to observable scales.

What would settle it

Detection of unsuppressed non-Bunch-Davies features in the CMB power spectrum or bispectrum at scales that should be exponentially screened by the known number of inflationary e-folds would contradict the screening claim.

Figures

Figures reproduced from arXiv: 2605.04166 by Chengxun Yuan, Farruh Atamurotov, G. Mustafa, Imtiaz Khan, Pirzada.

**Figure 1.** Figure 1: FIG. 1. Screening bounds for the pivot-scale scalar-power distortion. view at source ↗

**Figure 2.** Figure 2: FIG. 2. Visibility phase diagram for Euclidean-matched initial states. Left: maximal scalar-power memory for the Gaussian representative view at source ↗

**Figure 3.** Figure 3: FIG. 3. Left: sample spectra for the stretched-exponential filter with view at source ↗

read the original abstract

Euclidean wormholes can prepare inflation in non--Bunch--Davies initial states, but long Lorentzian expansion screens this memory from the CMB. We derive a visibility bound for Euclidean-matched Bogoliubov data: the pivot excitation satisfies $|\beta_*| \lesssim e^{-2N_{\rm pre}}$, and smooth Euclidean filters confine residual signatures to a comoving edge $k_w=a_iM$. Only near-minimal inflation, or an edge inside the observable window, leaves detectable scalar, tensor, and higher-point imprints. For longer inflation, wormhole-prepared perturbations are driven to the Bunch--Davies prediction. Euclidean memory therefore, becomes a quantitative bound on inflationary duration, with direct targets in CMB polarization and large-scale structure: the longer inflation lasts, the less of the wormhole remains on the sky.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

Long inflation erases detectable wormhole initial-state memory via an explicit exponential bound on the Bogoliubov coefficient.

read the letter

The main thing to know is that this paper derives a quantitative bound showing how long inflation must last to screen out any initial state signatures from Euclidean wormholes, driving the perturbations to the standard Bunch-Davies form. It takes the concept of wormhole-prepared non-Bunch-Davies states and matches them via Bogoliubov coefficients to the inflationary evolution. From there it gets the visibility bound on the pivot excitation |β_*| ≲ e^{-2N_pre}. The smooth filters then set a comoving edge scale k_w = a_i M beyond which nothing remains visible. This is new in providing an explicit link between the duration of inflation and the absence of detectable scalar, tensor, or higher-point imprints from the wormhole. What the paper does well is make the screening effect concrete and tied to observables. It points to CMB polarization and large-scale structure as places where near-minimal inflation might still show something if the edge falls inside the window. The logic is direct: more e-folds mean stronger suppression, so the memory fades. The soft spots are minor but worth noting. The whole bound depends on the details of how the Euclidean data is matched and how smooth the filters really are. If those are varied, the numerical factor in the exponent or the position of the edge could change. The paper presents this as a derived result without much exploration of alternatives, so the strength is in the specific case rather than a general proof. There are no obvious internal contradictions, and the conclusion follows from the premises. This paper is for cosmologists interested in quantum gravity effects on the early universe and how they might be constrained by data. Someone working on initial conditions for inflation or looking for ways to test non-standard vacua would find the targets useful, even if they don't agree with the wormhole setup. I recommend sending it to peer review. The work is focused and the argument is consistent enough that referees can evaluate the technical steps and suggest improvements on the assumptions.

Referee Report

2 major / 2 minor

Summary. The manuscript claims that Euclidean wormholes can prepare inflation in non-Bunch-Davies initial states, but long Lorentzian expansion screens this memory from the CMB. It derives a visibility bound for Euclidean-matched Bogoliubov data: the pivot excitation satisfies |β_*| ≲ e^{-2N_pre}, and smooth Euclidean filters confine residual signatures to a comoving edge k_w = a_i M. Only near-minimal inflation, or an edge inside the observable window, leaves detectable scalar, tensor, and higher-point imprints; for longer inflation, wormhole-prepared perturbations are driven to the Bunch-Davies prediction, turning the absence of such signatures into a quantitative lower bound on inflationary duration with targets in CMB polarization and large-scale structure.

Significance. If the central derivation holds, the result strengthens the robustness of standard inflationary predictions against quantum-gravity initial conditions and supplies a concrete, falsifiable link between Euclidean wormhole geometries and observable cosmology. It converts the lack of non-Bunch-Davies features into a direct constraint on the total number of e-folds, offering specific observational handles in CMB B-modes and LSS bispectra.

major comments (2)

[Derivation of the visibility bound (around Eq. for β_*)] The visibility bound |β_*| ≲ e^{-2N_pre} is expressed directly in terms of the pre-inflationary e-fold count N_pre. The manuscript must demonstrate explicitly (e.g., in the Bogoliubov-matching section) that this exponential suppression is an output of the Euclidean-to-Lorentzian matching and filter smoothness rather than an input assumption about the duration before the observable window begins.
[Filter construction and mode matching] The comoving edge k_w = a_i M is stated to arise from smooth Euclidean filters, but the text should provide the explicit filter function and the resulting mode suppression to confirm that this scale lies outside the observable window for N_pre ≳ 10 and does not introduce additional free parameters.

minor comments (2)

[Abstract] The abstract summarizes the bound cleanly but omits any reference to the section or equation number where the derivation appears; adding this would improve readability.
[Notation and definitions] Notation for N_pre and the pivot scale should be defined at first use and used consistently; a short table of symbols would help.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their positive assessment and constructive comments. The manuscript derives the visibility bound and filter scale from the Euclidean-to-Lorentzian matching; we address the requests for explicit demonstration below and will incorporate clarifications in the revised version.

read point-by-point responses

Referee: [Derivation of the visibility bound (around Eq. for β_*)] The visibility bound |β_*| ≲ e^{-2N_pre} is expressed directly in terms of the pre-inflationary e-fold count N_pre. The manuscript must demonstrate explicitly (e.g., in the Bogoliubov-matching section) that this exponential suppression is an output of the Euclidean-to-Lorentzian matching and filter smoothness rather than an input assumption about the duration before the observable window begins.

Authors: The bound is derived as an output of the matching. In the Bogoliubov section, the coefficients are obtained by integrating the Euclidean wormhole modes against the Lorentzian solutions across the filter; the resulting |β_*| acquires the factor e^{-2N_pre} from the exponential decay of the sub-horizon modes during the pre-inflationary expansion. This follows directly from the smoothness of the filter and the WKB suppression in the mode equation, without presupposing the value of N_pre. We will insert the intermediate steps of this integral in the revised manuscript to make the derivation fully explicit. revision: yes
Referee: [Filter construction and mode matching] The comoving edge k_w = a_i M is stated to arise from smooth Euclidean filters, but the text should provide the explicit filter function and the resulting mode suppression to confirm that this scale lies outside the observable window for N_pre ≳ 10 and does not introduce additional free parameters.

Authors: We agree that the explicit form strengthens clarity. The filter is the Gaussian F(k) = exp[−(k/(a_i M))^2], chosen to match the Euclidean wormhole regularity; the resulting Bogoliubov coefficients are exponentially suppressed for k ≫ a_i M. For N_pre ≳ 10 the comoving edge k_w is stretched by e^{N_pre} to scales far outside the observable window, with no additional parameters introduced beyond the geometric scale M fixed by the wormhole. We will add the explicit filter expression, the suppressed mode functions, and a brief calculation confirming the location of k_w in the revised text. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation is self-contained from standard inflationary dynamics.

full rationale

The claimed visibility bound |β_*| ≲ e^{-2N_pre} and edge k_w = a_i M are derived from Bogoliubov matching of Euclidean wormhole states to Lorentzian inflation followed by the exponential stretching of modes during expansion. This is a direct consequence of the mode evolution equations under the given assumptions and does not reduce any output quantity to a fitted input or self-citation by construction. N_pre enters as the duration parameter whose effect is being quantified, not as a hidden fit; the screening to Bunch-Davies is the expected outcome once the matching and filter smoothness are granted. No self-definitional, fitted-prediction, or uniqueness-imported steps appear in the abstract or described chain.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review supplies insufficient detail to enumerate free parameters, axioms, or invented entities with precision; the bound references N_pre and k_w but their status (fitted vs. derived) is not stated.

pith-pipeline@v0.9.0 · 5445 in / 1352 out tokens · 90067 ms · 2026-05-08T17:46:24.936335+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith.Cost (J = ½(x+x⁻¹)−1) washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

We derive a visibility bound for Euclidean-matched Bogoliubov data: the pivot excitation satisfies |β_*| ≲ e^{-2N_pre}, and smooth Euclidean filters confine residual signatures to a comoving edge k_w = a_i M.
IndisputableMonolith.Foundation.BranchSelection branch_selection (free family parameter ν, c — RS forbids such freedom in calibrated cost) unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

β(p) = β_0 e^{iθ_0} exp[−(p/M)^ν], ν > 0, which interpolates between exponential, Gaussian, and super-Gaussian damping.
IndisputableMonolith.Foundation.Breath1024 (8-tick / φ-ladder spacings) n/a — paper's e-fold counter is not an RS tick orbit unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

k_w ≡ a_i M = k_* (M/H_*) e^{-N_pre}; for N_pre exceeding ln(M/H_*) + O(1) the pivot is screened.

What do these tags mean?

matches: The paper's claim is directly supported by a theorem in the formal canon.
supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

46 extracted references · 40 canonical work pages · 3 internal anchors

[1]

A. H. Guth, The Inflationary Universe: A Possible Solution to the Horizon and Flatness Problems, Phys. Rev. D23, 347 (1981)

1981
[2]

V . F. Mukhanov and G. V . Chibisov, Quantum Fluctuations and a Nonsingular Universe, JETP Lett.33, 532 (1981)

1981
[3]

Chen, K.-N

P. Chen, K.-N. Lin, W.-C. Lin, and D.-h. Yeom, Possible origin ofα-vacua as the initial state of the Universe, Phys. Rev. D111, 083520 (2025), arXiv:2404.15450 [gr-qc]

work page arXiv 2025
[4]

P. Chen, D. Ro, and D.-h. Yeom, Fuzzy Euclidean wormholes in the inflationary universe, Phys. Dark Univ.28, 100492 (2020), arXiv:1904.00199 [gr-qc]

work page arXiv 2020
[5]

Betzios and O

P. Betzios and O. Papadoulaki, Inflationary Cosmology from Anti-de Sitter Wormholes, Phys. Rev. Lett.133, 021501 (2024), arXiv:2403.17046 [hep-th]. 5

work page arXiv 2024
[6]

Prepare inflationary universe via the Euclidean charged wormhole,

Q.-Y . Lan and Y .-S. Piao, Prepare inflationary universe via the Euclidean charged wormhole, arXiv preprint (2024), arXiv:2411.13844 [gr-qc]

work page arXiv 2024
[7]

Betzios, I

P. Betzios, I. D. Gialamas, and O. Papadoulaki, Magnetic anti–de Sitter wormholes as seeds for Higgs inflation, Phys. Rev. D111, 123542 (2025), arXiv:2412.03639 [hep-th]

work page arXiv 2025
[8]

Lavrelashvili and J.-L

G. Lavrelashvili and J.-L. Lehners, Nucleating an Inflationary Universe: Euclidean Wormholes and their No-Boundary Limit, arXiv preprint (2026), arXiv:2603.11003 [hep-th]

work page arXiv 2026
[9]

Goldstein and D

K. Goldstein and D. A. Lowe, A Note on alpha vacua and in- teracting field theory in de Sitter space, Nucl. Phys. B669, 325 (2003), arXiv:hep-th/0302050

work page arXiv 2003
[10]

Collins, R

H. Collins, R. Holman, and M. R. Martin, The Fate of the alpha vacuum, Phys. Rev. D68, 124012 (2003), arXiv:hep- th/0306028

work page arXiv 2003
[11]

Collins and R

H. Collins and R. Holman, Taming the alpha vacuum, Phys. Rev. D70, 084019 (2004), arXiv:hep-th/0312143

work page arXiv 2004
[12]

M. B. Einhorn and F. Larsen, Squeezed states in the de Sit- ter vacuum, Phys. Rev. D68, 064002 (2003), arXiv:hep- th/0305056

work page arXiv 2003
[13]

Brunetti, K

R. Brunetti, K. Fredenhagen, and S. Hollands, A Remark on alpha vacua for quantum field theories on de Sitter space, JHEP 05(05), 063, arXiv:hep-th/0503022

work page arXiv
[14]

Parker and S

L. Parker and S. A. Fulling, Quantized matter fields and the avoidance of singularities in general relativity, Phys. Rev. D7, 2357 (1973)

1973
[15]

N. D. Birrell and P. C. W. Davies,Quantum Fields in Curved Space, Cambridge Monographs on Mathematical Physics (Cambridge University Press, Cambridge, UK, 1982)

1982
[16]

Pirzada, I. Khan, M. Khan, T. Li, and A. Muhammad, Non- Minimal Dilaton Inflation from the Effective Gluodynamics, arXiv preprint (2026), arXiv:2603.00818 [hep-ph]

work page arXiv 2026
[17]

Martin and R

J. Martin and R. H. Brandenberger, The TransPlanckian prob- lem of inflationary cosmology, Phys. Rev. D63, 123501 (2001), arXiv:hep-th/0005209

work page arXiv 2001
[18]

Easther, B

R. Easther, B. R. Greene, W. H. Kinney, and G. Shiu, A Generic estimate of transPlanckian modifications to the pri- mordial power spectrum in inflation, Phys. Rev. D66, 023518 (2002), arXiv:hep-th/0204129

work page arXiv 2002
[19]

U. H. Danielsson, A Note on inflation and transPlanck- ian physics, Phys. Rev. D66, 023511 (2002), arXiv:hep- th/0203198

work page arXiv 2002
[20]

Kaloper, M

N. Kaloper, M. Kleban, A. Lawrence, S. Shenker, and L. Susskind, Initial conditions for inflation, JHEP11(11), 037, arXiv:hep-th/0209231

work page arXiv
[21]

Goldstein and D

K. Goldstein and D. A. Lowe, Initial state effects on the cosmic microwave background and transPlanckian physics, Phys. Rev. D67, 063502 (2003), arXiv:hep-th/0208167

work page arXiv 2003
[22]

M. Porrati, Effective field theory approach to cosmological ini- tial conditions: Self-consistency bounds and non-Gaussianities, in13th International Seminar on High-Energy Physics: Quarks 2004(2004) arXiv:hep-th/0409210

work page internal anchor Pith review arXiv 2004
[23]

Enhanced Non-Gaussianity from Excited Initial States

R. Holman and A. J. Tolley, Enhanced Non-Gaussianity from Excited Initial States, JCAP05(05), 001, arXiv:0710.1302 [hep-th]

work page arXiv
[24]

O’Connell and R

R. O’Connell and R. Holman, Initial Conditions in the Ef- fective Field Theory of Inflation, arXiv preprint (2011), arXiv:1109.1562 [hep-th]

work page arXiv 2011
[25]

Carney, W

D. Carney, W. Fischler, S. Paban, and N. Sivanandam, The Inflationary Wavefunction and its Initial Conditions, JCAP12 (12), 012, arXiv:1109.6566 [hep-th]

work page arXiv
[26]

Kundu, Inflation with General Initial Conditions for Scalar Perturbations, JCAP02(02), 005, arXiv:1110.4688 [astro- ph.CO]

S. Kundu, Inflation with General Initial Conditions for Scalar Perturbations, JCAP02(02), 005, arXiv:1110.4688 [astro- ph.CO]

work page arXiv
[27]

Aravind, D

A. Aravind, D. Lorshbough, and S. Paban, Non-Gaussianity from Excited Initial Inflationary States, JHEP07(07), 076, arXiv:1303.1440 [hep-th]

work page arXiv
[28]

R. H. Brandenberger and J. Martin, Trans-Planckian Issues for Inflationary Cosmology, Class. Quant. Grav.30, 113001 (2013), arXiv:1211.6753 [astro-ph.CO]

work page arXiv 2013
[29]

P. D. Meerburg, J. P. van der Schaar, and P. S. Corasaniti, Sig- natures of Initial State Modifications on Bispectrum Statistics, JCAP05(05), 018, arXiv:0901.4044 [hep-th]

work page arXiv
[30]

Ganc, Calculating the local-type fNL for slow-roll infla- tion with a non-vacuum initial state, Phys

J. Ganc, Calculating the local-type fNL for slow-roll infla- tion with a non-vacuum initial state, Phys. Rev. D84, 063514 (2011), arXiv:1104.0244 [astro-ph.CO]

work page arXiv 2011
[31]

Flauger, D

R. Flauger, D. Green, and R. A. Porto, On squeezed lim- its in single-field inflation. Part I, JCAP08(08), 032, arXiv:1303.1430 [hep-th]

work page arXiv
[32]

Kanno,Nonclassical primordial gravitational waves from the initial entangled state,Phys

S. Kanno, Nonclassical primordial gravitational waves from the initial entangled state, Phys. Rev. D100, 123536 (2019), arXiv:1905.06800 [hep-th]

work page arXiv 2019
[33]

Kanno and M

S. Kanno and M. Sasaki, Graviton non-gaussianity inα- vacuum, JHEP08(08), 210, arXiv:2206.03667 [hep-th]

work page arXiv
[34]

A. J. Chopping, C. Sleight, and M. Taronna, Cosmological correlators for Bogoliubov initial states, JHEP09(09), 152, arXiv:2407.16652 [hep-th]

work page arXiv
[35]

Ghosh, E

D. Ghosh, E. Pajer, and F. Ullah, Cosmological cutting rules for Bogoliubov initial states, SciPost Phys.18, 005 (2025), arXiv:2407.06258 [hep-th]

work page arXiv 2025
[36]

Ghosh and F

D. Ghosh and F. Ullah, Cosmological cutting rules for Bogoli- ubov initial states: any mass and spin, JCAP09(09), 016, arXiv:2502.05630 [hep-th]

work page arXiv
[37]

ACT-ing on inflation: Implications of non Bunch-Davies initial condition and reheating on single-field slow roll models

S. Maity, ACT-ing on inflation: Implications of non bunch- Davies initial condition and reheating on single-field slow roll models, Phys. Lett. B870, 139913 (2025), arXiv:2505.10534 [astro-ph.CO]

work page internal anchor Pith review Pith/arXiv arXiv 2025
[38]

T. S. Bunch and P. C. W. Davies, Quantum Field Theory in de Sitter Space: Renormalization by Point Splitting, Proc. Roy. Soc. Lond. A360, 117 (1978)

1978
[39]

Allen, Vacuum States in de Sitter Space, Phys

B. Allen, Vacuum States in de Sitter Space, Phys. Rev. D32, 3136 (1985)

1985
[40]

Planck 2018 results. X. Constraints on inflation

Y . Akramiet al.(Planck), Planck 2018 results. X. Con- straints on inflation, Astron. Astrophys.641, A10 (2020), arXiv:1807.06211 [astro-ph.CO]

work page internal anchor Pith review arXiv 2018
[41]

Ganc and E

J. Ganc and E. Komatsu, Scale-dependent bias of galaxies and mu-type distortion of the cosmic microwave background spectrum from single-field inflation with a modified initial state, Phys. Rev. D86, 023518 (2012), arXiv:1204.4241 [astro- ph.CO]

work page arXiv 2012
[42]

Emami, E

R. Emami, E. Dimastrogiovanni, J. Chluba, and M. Kamionkowski, Probing the scale dependence of non- Gaussianity with spectral distortions of the cosmic mi- crowave background, Phys. Rev. D91, 123531 (2015), arXiv:1504.00675 [astro-ph.CO]

work page arXiv 2015
[43]

Schöneberg, M

N. Schöneberg, M. Lucca, and D. C. Hooper, Constraining the inflationary potential with spectral distortions, JCAP03(03), 036, arXiv:2010.07814 [astro-ph.CO]

work page arXiv 2010
[44]

X. Chen, P. D. Meerburg, and M. Münchmeyer, The Future of Primordial Features with 21 cm Tomography, JCAP09(09), 023, arXiv:1605.09364 [astro-ph.CO]

work page arXiv
[45]

S. S. Naik, P. Chingangbam, S. Singh, A. Mesinger, and K. Fu- ruuchi, Global 21 cm signal: a promising probe of primordial features, JCAP05(05), 038, arXiv:2501.02538 [astro-ph.CO]

work page arXiv
[46]

Swampland distance conjecture, inflation andα-attractors,

M. Scalisi and I. Valenzuela, Swampland distance con- jecture, inflation andα-attractors, JHEP08(08), 160, arXiv:1812.07558 [hep-th]. 6 SUPPLEMENTAL MATERIAL: LONG INFLATION SCREENS EUCLIDEAN-WORMHOLE INITIAL STATES This Supplemental Material gives the Euclidean matching construction, the finite-energy screening bounds used in the Letter, and the formulas...

work page arXiv