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arxiv: 2605.30259 · v1 · pith:UU47VQRAnew · submitted 2026-05-28 · 🌌 astro-ph.CO · hep-ph· hep-th

Late-time Quantum Vacuum Decay and its Cosmological Implications

Yang Bai , Sida Lu , Nicholas Orlofsky This is my paper

Pith reviewed 2026-06-29 05:37 UTC · model grok-4.3

classification 🌌 astro-ph.CO hep-phhep-th
keywords late-time quantum vacuum decayquantum tunnelingcosmological observablesdark matter conversiondomain wallsbaryon acoustic oscillationsCMB anisotropiesvacuum energy
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The pith

Cosmological distance and CMB data still permit a 50 percent drop in vacuum energy from late-time quantum tunneling at redshift below 1.

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

The paper builds phenomenological models in which the universe tunnels between metastable vacua at late times, lowering vacuum energy and possibly converting a fraction of dark matter into radiation while producing domain walls. These models generate altered expansion histories that are compared directly to DESI baryon acoustic oscillation measurements, multiple supernova distance catalogs, and a compressed CMB likelihood. Current data leave room for a 50 percent vacuum-energy decrease when the transition occurs at redshift less than 1. One variant that includes dark-matter conversion and domain-wall production fits the observations better than the standard Lambda-CDM model, favoring a transition near redshift 7 with roughly 10 percent of dark matter participating. CMB anisotropy limits from bubble nucleation and domain-wall networks restrict slow transitions but can be avoided when tunneling depends on dark-matter density.

Core claim

Late-time quantum vacuum decay remains compatible with existing cosmological data. For minimal tunneling models a 50 percent drop in total vacuum energy is still allowed at transition redshifts below 1. The model that adds dark-matter conversion and domain-wall production yields a good fit that eases tensions with Lambda-CDM, preferring a transition redshift near 7 and participation of about 10 percent of the dark matter. CMB constraints from bubble nucleation and the resulting domain-wall network limit slow or sparse transitions to an O(10 percent) vacuum-energy change at order-unity redshift, while nonminimal models with dark-matter-density-dependent tunneling rates can evade these limits.

What carries the argument

Phenomenological parametrization of a vacuum-energy drop at transition redshift z_t together with a dark-matter conversion fraction and an accompanying domain-wall network.

If this is right

  • Current distance measurements still allow a 50 percent decrease in total vacuum energy for any transition redshift below 1.
  • The dark-matter conversion plus domain-wall model resolves cosmological tensions with a preferred transition at z_t approximately 7 and 10 percent dark-matter participation.
  • CMB anisotropy limits from bubble nucleation restrict slow or sparse late transitions to an O(10 percent) vacuum-energy change at order-unity redshift.
  • Dark-matter-density-dependent tunneling can proceed rapidly enough to evade the CMB bounds that apply to slower transitions.

Where Pith is reading between the lines

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

  • More precise future distance surveys could detect or exclude the specific expansion-history features predicted by the favored transition parameters.
  • The same framework offers a direct observational test of metastable-vacuum scenarios motivated by landscape constructions.
  • Similar phenomenological modeling could be applied to other late-time phase transitions that alter dark-sector energy densities.

Load-bearing premise

The chosen parametrization of the vacuum-energy drop, dark-matter conversion fraction, and domain-wall network accurately captures the late-time tunneling process without a full quantum-field-theory calculation of the tunneling rate or bubble dynamics.

What would settle it

A future measurement of the expansion history at redshift around 7 that shows no deviation from Lambda-CDM and no sign of the 10 percent dark-matter conversion would rule out the parameters preferred by the best-fit model.

Figures

Figures reproduced from arXiv: 2605.30259 by Nicholas Orlofsky, Sida Lu, Yang Bai.

Figure 1
Figure 1. Figure 1: Schematic illustration of quantum tunneling in vacuum decay. The circle denotes a [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The numerically obtained four-dimensional Euclidean action [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Hubble diagrams showing the comparison of [PITH_FULL_IMAGE:figures/full_fig_p017_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Posterior distribution for the parameters in the QT model for the likelihood combi [PITH_FULL_IMAGE:figures/full_fig_p022_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p023_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p025_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Schematic illustration of the effect on CMB photons of a phase transition. Bubbles [PITH_FULL_IMAGE:figures/full_fig_p028_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Left: The single-bubble (blue) and double-bubble (orange) contributions to ⟨δtc(x)δtc(y)⟩. Their sum is shown in green. Right: Pδt(k) for the combined single- and double￾bubble contributions. H(tp)γ −1/4 is taken to be unity for plotting purposes. and ΩΛ + Ωm ≈ 1 had been assumed. Its derivation is given in Appendix C. In the following, we will approximate the redshift at which the PT completes to be the s… view at source ↗
Figure 9
Figure 9. Figure 9: The CMB temperature power spectrum for various values of [PITH_FULL_IMAGE:figures/full_fig_p031_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Bounds on r = ΩV /(ΩΛ,0 + ΩV ) and zt . The solid lines show the exclusion bounds for vacuum PTs with various values of ΩΛ = ΩΛ,0 + ΩV ; excluded regions are to the top-left of these lines. The dot-dashed lines show exclusion bounds for PTs with time-dependent nucleation rates with various values of β/H, fixing ΩΛ = 0.69. For all, Ωm = 0.31. The triangles terminating on lines (◁) show the minimum value of… view at source ↗
read the original abstract

The existence of a landscape of metastable vacua raises the possibility that our Universe may have undergone quantum vacuum decay at late times. This work explores how such a transition can be tested with cosmological observables, focusing on precision distance measurements and cosmic microwave background (CMB) anisotropies. A set of phenomenological models is constructed in which late-time quantum tunneling changes the vacuum energy and may convert a subcomponent of dark matter into dark radiation, possibly accompanied by domain-wall production. The resulting expansion histories are compared with DESI DR2 baryon acoustic oscillation data; supernova distance measurements from DES-Dovekie, Pantheon+, and Union3; and a compressed CMB likelihood. For quantum-tunneling models, current cosmological distance measurements still allow a 50% decrease in the total vacuum energy for a transition redshift $z_t<1$. The model with dark-matter conversion and domain-wall production provides a good fit to resolve the tension between cosmological observables and the $\Lambda$CDM model, with a preferred transition around $z_t \sim 7$ and about 10% of dark matter participating in the transition. Additionally, CMB anisotropy constraints from bubble nucleation and the associated domain-wall network are derived and shown to strongly restrict slow or sparse late transitions. Applied to the minimal quantum-tunneling model, these constraints allow an $\mathcal{O}(10\%)$ decrease in the total vacuum energy for a transition redshift $z_t$ of order unity. For nonminimal models, dark-matter-density-dependent tunneling can proceed rapidly enough to evade such bounds. These results demonstrate that late-time quantum vacuum decay is a testable cosmological phenomenon and provide a concrete observational handle on metastable-vacuum physics motivated by landscape scenarios.

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.

Referee Report

3 major / 2 minor

Summary. The paper explores late-time quantum vacuum decay in metastable vacua motivated by landscape scenarios. It introduces phenomenological models in which tunneling alters vacuum energy (possibly by up to 50%), converts a fraction of dark matter to dark radiation, and produces domain walls. Expansion histories are inserted into the Friedmann equation and compared to DESI DR2 BAO, DES-Dovekie/Pantheon+/Union3 supernovae, and compressed CMB data. The abstract reports that current data still permit a 50% vacuum-energy drop for z_t < 1, while a non-minimal model with ~10% DM conversion at z_t ~ 7 yields a good fit that resolves cosmological tensions; CMB anisotropy bounds from nucleation and domain walls are also derived and shown to restrict slow transitions.

Significance. If the parametrizations can be justified microphysically, the work supplies a concrete observational test of landscape-motivated vacuum decay and shows that existing distance and CMB data already constrain the allowed parameter space. The approach is novel in combining vacuum-energy drop, DM conversion, and domain-wall production, but its significance is limited by the absence of first-principles derivations of the tunneling rate or bubble dynamics.

major comments (3)
  1. [Abstract / Model Construction] Abstract and model-construction paragraphs: the expansion histories are inserted directly into the Friedmann equation without a derivation of the nucleation rate Γ from an instanton or Coleman–De Luccia calculation for a potential that would produce transitions at z ~ O(1) or z ~ 7. This is load-bearing for the claim that the models are motivated by landscape physics rather than chosen to fit data.
  2. [Abstract] Abstract: the statements that the model 'provides a good fit' with 'preferred' z_t ~ 7 and 10% DM conversion are obtained by fitting the free parameters (z_t, vacuum-energy drop fraction, DM conversion fraction) to the same DESI + supernova + CMB datasets used to claim tension resolution. This circularity undermines the interpretation of these values as independent predictions or resolutions.
  3. [CMB Constraints] CMB anisotropy constraints paragraph: bounds on bubble nucleation and domain-wall networks are computed within the same phenomenological parametrization rather than from first-principles wall velocity, percolation, or early-universe stability requirements. If the microphysical rate cannot reach the required values without violating other constraints, the allowed O(10%) vacuum-energy drop for z_t ~ 1 collapses.
minor comments (2)
  1. [Model Construction] Notation for the domain-wall tension and its time dependence should be defined explicitly when first introduced.
  2. [Abstract] The abstract refers to 'compressed CMB likelihood' without specifying which likelihood or compression method is used.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive report. Below we address each major comment directly, clarifying the scope and intent of our phenomenological analysis while acknowledging its limitations.

read point-by-point responses

  1. Referee: [Abstract / Model Construction] Abstract and model-construction paragraphs: the expansion histories are inserted directly into the Friedmann equation without a derivation of the nucleation rate Γ from an instanton or Coleman–De Luccia calculation for a potential that would produce transitions at z ~ O(1) or z ~ 7. This is load-bearing for the claim that the models are motivated by landscape physics rather than chosen to fit data.

    Authors: The manuscript is explicitly phenomenological, as stated in the introduction and model sections. Landscape scenarios supply the general motivation that metastable vacua can exist and decay at late times, but we do not derive a specific instanton or Coleman–De Luccia rate. The parametrization of z_t, vacuum-energy drop, and DM conversion fraction is chosen to explore observable consequences within current data. This approach tests whether such transitions remain viable, without claiming a first-principles derivation of the rate. We will add an explicit sentence in the model-construction paragraph reiterating that the work does not provide a microphysical potential. revision: partial

  2. Referee: [Abstract] Abstract: the statements that the model 'provides a good fit' with 'preferred' z_t ~ 7 and 10% DM conversion are obtained by fitting the free parameters (z_t, vacuum-energy drop fraction, DM conversion fraction) to the same DESI + supernova + CMB datasets used to claim tension resolution. This circularity undermines the interpretation of these values as independent predictions or resolutions.

    Authors: The quoted phrasing reports the best-fit values obtained from the joint likelihood analysis. These values illustrate that parameter choices exist within the model that improve the fit relative to ΛCDM and reduce certain tensions. The exercise is not presented as an independent prediction but as a demonstration of consistency and possible tension alleviation. Any fitted model necessarily uses the same data for both fitting and comparison; the scientific content lies in mapping the allowed parameter space and its implications for observables. revision: no

  3. Referee: [CMB Constraints] CMB anisotropy constraints paragraph: bounds on bubble nucleation and domain-wall networks are computed within the same phenomenological parametrization rather than from first-principles wall velocity, percolation, or early-universe stability requirements. If the microphysical rate cannot reach the required values without violating other constraints, the allowed O(10%) vacuum-energy drop for z_t ~ 1 collapses.

    Authors: The CMB bounds are derived from the phenomenological parameters (transition redshift, participating DM fraction, and implied nucleation rate) and are therefore model-dependent. We present them as indicative constraints within this framework rather than absolute limits. The text already notes that density-dependent tunneling in non-minimal models can produce sufficiently rapid transitions to evade the bounds. A full first-principles calculation would require a specific potential, which lies outside the scope of the present work; the current bounds serve to restrict the slow-transition regime of the phenomenological models. revision: no

Circularity Check

0 steps flagged

No circularity: phenomenological parametrization fitted directly to external data

full rationale

The paper constructs explicit phenomenological models for vacuum-energy drop, DM conversion, and domain walls, then compares the resulting Friedmann-equation expansion histories to independent datasets (DESI DR2 BAO, DES-Dovekie/Pantheon+/Union3 supernovae, compressed CMB). The reported allowances (50% vacuum-energy drop for z_t<1) and best-fit values (z_t~7, ~10% DM conversion) are outputs of this data comparison, not inputs redefined as predictions. No equation or section reduces a claimed first-principles result to a fitted parameter or self-citation; the text labels the models as phenomenological and derives CMB bubble-nucleation bounds within the same parametrization without claiming microphysical derivation from instantons. The analysis is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 1 invented entities

The central claims rest on standard FLRW cosmology plus three fitted quantities (transition redshift z_t, vacuum-energy drop fraction, dark-matter conversion fraction) and the assumption that bubble nucleation and domain-wall networks produce only the stated CMB signatures. No machine-checked derivations or external benchmarks are referenced.

free parameters (3)
  • transition redshift z_t
    Chosen to fit distance and CMB data; appears as a free parameter in all models.
  • vacuum-energy drop fraction
    Fitted; the abstract states that a 50% drop remains allowed for z_t < 1.
  • dark-matter conversion fraction
    Fitted; ~10% preferred in the non-minimal model.
axioms (2)
  • domain assumption Late-time quantum tunneling can be modeled by a sudden change in vacuum energy at a single redshift without back-reaction on the metric or particle content beyond the stated conversion.
    Invoked when constructing the set of phenomenological models.
  • standard math Standard ΛCDM background plus linear perturbations remain valid when domain walls are produced.
    Required for the CMB anisotropy constraints.
invented entities (1)
  • late-time domain-wall network no independent evidence
    purpose: Produced during the tunneling transition and used to generate additional CMB constraints.
    Introduced in the non-minimal model; no independent evidence outside the fit is provided.

pith-pipeline@v0.9.1-grok · 5840 in / 1757 out tokens · 21360 ms · 2026-06-29T05:37:26.544056+00:00 · methodology

discussion (0)

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Forward citations

Cited by 1 Pith paper

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