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arxiv: 2507.23355 · v2 · pith:XBBFUUN6new · submitted 2025-07-31 · 🌌 astro-ph.CO · gr-qc

SPT-3G D1: Axion Early Dark Energy with CMB experiments and DESI

A. R. Khalife , L. Balkenhol , E. Camphuis , A. J. Anderson , B. Ansarinejad , M. Archipley , P. S. Barry , K. Benabed
show 87 more authors
A. N. Bender B. A. Benson F. Bianchini L. E. Bleem F. R. Bouchet L. Bryant M. G. Campitiello J. E. Carlstrom C. L. Chang P. Chaubal P. M. Chichura A. Chokshi T. L. Chou A. Coerver T. M. Crawford C. Daley T. de Haan K. R. Dibert M. A. Dobbs M. Doohan A. Doussot D. Dutcher W. Everett C. Feng K. R. Ferguson K. Fichman A. Foster S. Galli A. E. Gambrel R. W. Gardner F. Ge N. Goeckner-Wald R. Gualtieri F. Guidi S. Guns N. W. Halverson E. Hivon W. L. Holzapfel J. C. Hood A. Hryciuk N. Huang F. K\'eruzor\'e L. Knox M. Korman K. Kornoelje C. L. Kuo K. Levy A. E. Lowitz C. Lu G. P. Lynch A. Maniyar E. S. Martsen F. Menanteau M. Millea J. Montgomery Y. Nakato T. Natoli G. I. Noble Y. Omori A. Ouellette Z. Pan P. Paschos K. A. Phadke A. W. Pollak K. Prabhu W. Quan M. Rahimi A. Rahlin C. L. Reichardt M. Rouble J. E. Ruhl E. Schiappucci A. Simpson J. A. Sobrin A. A. Stark J. Stephen C. Tandoi B. Thorne C. Trendafilova C. Umilta J. D. Vieira A. Vitrier Y. Wan N. Whitehorn W. L. K. Wu M. R. Young J. A. Zebrowski (for the SPT-3G Collaboration)
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Pith reviewed 2026-05-21 23:31 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qc
keywords axion early dark energyHubble tensionCMBDESIBAOcosmological constraintsSPTACT
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The pith

DESI data combined with CMB observations yields mild preference for axion early dark energy and reduces the Hubble tension to 2.6 sigma.

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

The paper updates constraints on axion early dark energy by combining measurements from the South Pole Telescope, Atacama Cosmology Telescope, Planck, and baryon acoustic oscillations from DESI. CMB data alone show no significant evidence for this component and only moderate relief to the Hubble tension. Adding DESI data produces a weak statistical preference for a small positive contribution from axion early dark energy, which shifts the inferred expansion rate and brings the tension down to 2.6 sigma. A reader would care because the result illustrates how an existing mismatch between current datasets can favor a specific early-universe extension when the datasets are joined.

Core claim

Combining DESI BAO measurements with CMB data from SPT, ACT, and Planck gives f_EDE = 0.055^{+0.024}_{-0.047} at 68% CL together with a weak preference for the axion early dark energy model over Lambda CDM; this combination reduces the Hubble tension to 2.6 sigma. CMB-only analyses find no statistically significant evidence for AEDE and only moderate tension reduction, while the parameter shift upon adding DESI traces directly to the discrepancy between DESI and CMB measurements already present in the baseline Lambda CDM model.

What carries the argument

Axion early dark energy (AEDE), a model in which a light axion field contributes a fractional energy density f_EDE near matter-radiation equality and thereby alters the sound horizon scale.

If this is right

  • SPT data alone limit f_EDE below 0.12 at 95% CL and reduce the Hubble tension to 2.3 sigma.
  • The full CMB combination (SPT+ACT+Planck) limits f_EDE below 0.07 at 95% CL and leaves the tension at 3.6 sigma.
  • DESI plus SPT alone gives f_EDE = 0.081^{+0.037}_{-0.052} at 68% CL and lowers the tension to 1.5 sigma.
  • The reported shift occurs specifically because DESI and CMB disagree inside Lambda CDM.

Where Pith is reading between the lines

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

  • If the mild preference strengthens with future data releases, targeted axion searches in particle-physics experiments could become higher priority.
  • The same dataset tension could be tested by comparing AEDE against other early-dark-energy parameterizations to see which fits best.
  • Improved control of systematics in either DESI or CMB pipelines could remove the need for AEDE altogether.

Load-bearing premise

The discrepancy between DESI BAO measurements and CMB data in the standard Lambda CDM model is assumed to be best explained by adding axion early dark energy rather than by unaccounted systematics or other extensions.

What would settle it

A future high-precision BAO measurement that aligns DESI and CMB results inside Lambda CDM without any room for positive f_EDE would eliminate the reported preference.

Figures

Figures reproduced from arXiv: 2507.23355 by A. A. Stark, A. Chokshi, A. Coerver, A. Doussot, A. E. Gambrel, A. E. Lowitz, A. Foster, A. Hryciuk, A. J. Anderson, A. Maniyar, A. N. Bender, A. Ouellette, A. Rahlin, A. R. Khalife, A. Simpson, A. Vitrier, A. W. Pollak, B. A. Benson, B. Ansarinejad, B. Thorne, C. Daley, C. Feng, C. L. Chang, C. L. Kuo, C. L. Reichardt, C. Lu, C. Tandoi, C. Trendafilova, C. Umilta, D. Dutcher, E. Camphuis, E. Hivon, E. Schiappucci, E. S. Martsen, F. Bianchini, F. Ge, F. Guidi, F. K\'eruzor\'e, F. Menanteau, F. R. Bouchet, G. I. Noble, G. P. Lynch, J. A. Sobrin, J. A. Zebrowski (for the SPT-3G Collaboration), J. C. Hood, J. D. Vieira, J. E. Carlstrom, J. E. Ruhl, J. Montgomery, J. Stephen, K. A. Phadke, K. Benabed, K. Fichman, K. Kornoelje, K. Levy, K. Prabhu, K. R. Dibert, K. R. Ferguson, L. Balkenhol, L. Bryant, L. E. Bleem, L. Knox, M. A. Dobbs, M. Archipley, M. Doohan, M. G. Campitiello, M. Korman, M. Millea, M. Rahimi, M. Rouble, M. R. Young, N. Goeckner-Wald, N. Huang, N. W. Halverson, N. Whitehorn, P. Chaubal, P. M. Chichura, P. Paschos, P. S. Barry, R. Gualtieri, R. W. Gardner, S. Galli, S. Guns, T. de Haan, T. L. Chou, T. M. Crawford, T. Natoli, W. Everett, W. L. Holzapfel, W. L. K. Wu, W. Quan, Y. Nakato, Y. Omori, Y. Wan, Z. Pan.

Figure 1
Figure 1. Figure 1: FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Constraints in the [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Summary of the main results of this work. Shown are constraints, within AEDE, from [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Same as the top plot of Fig [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
read the original abstract

We present the most up-to-date constraints on axion early dark energy (AEDE) from cosmic microwave background (CMB) and baryon acoustic oscillation (BAO) measurements. In particular, we assess the impact of data from ground-based CMB experiments, the South Pole Telescope (SPT) and the Atacama Cosmology Telescope (ACT) -- both with and without $Planck$ -- on constraints on AEDE. We also highlight the impact that BAO information from the Dark Energy Spectroscopic Instrument (DESI) has on these constraints. From CMB data alone, we do not find statistically significant evidence for the presence of AEDE, and we find only moderate reduction in the Hubble tension. From the latest SPT data alone, we find the maximal fractional contribution of AEDE to the cosmic energy budget is $f_{\rm EDE}\,<\,0.12$ at $95\,$% confidence level (CL), and the Hubble tension between the SPT and SH0ES results is reduced to the $2.3\,\sigma$ level. When combining the latest SPT, ACT, and $Planck$ datasets, we find $f_{\rm EDE}\,<\,0.070$ at $95\,$% CL and the Hubble tension at the $3.6\, \sigma$ level. In contrast, adding DESI data to the CMB datasets results in mild preference for AEDE and, in some cases, non-negligible reduction in the Hubble tension. From SPT+DESI, we find $f_{\rm EDE}\,=\,0.081^{+0.037}_{-0.052}$ at $68\,$% CL, and the Hubble tension reduces to $1.5\,\sigma$. From the combination of DESI with all three CMB experiments, we get $f_{\rm EDE}\,=\, 0.055^{+0.024}_{-0.047}$ at $68\,$% CL and a weak preference for AEDE over $\Lambda$CDM. This data combination, in turn, reduces the Hubble tension to $2.6\, \sigma$. We highlight that this shift in parameters when adding the DESI dataset is a manifestation of the discrepancy currently present between DESI and CMB experiments in the concordance model $\Lambda$CDM.

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

1 major / 1 minor

Summary. The paper presents the most up-to-date constraints on axion early dark energy (AEDE) using CMB data from SPT-3G, ACT, and Planck (individually and combined) together with BAO measurements from DESI. CMB data alone show no statistically significant evidence for AEDE and only moderate reduction of the Hubble tension. Adding DESI data produces a mild preference for AEDE, with f_EDE = 0.055^{+0.024}_{-0.047} at 68% CL from the full CMB+DESI combination, a weak preference over ΛCDM, and reduction of the Hubble tension to 2.6σ; the authors attribute the parameter shift to the existing DESI-CMB discrepancy in baseline ΛCDM.

Significance. If the results hold, the work is significant because it supplies timely, multi-experiment constraints on AEDE using the latest ground-based CMB and DESI BAO data. The explicit comparison across data combinations and the clear statement that the shift is a manifestation of the known ΛCDM tension between DESI and CMB are useful for the community. The analysis employs standard cosmological likelihood methods and reports both upper limits and best-fit values with credible intervals.

major comments (1)
  1. [Abstract] Abstract: the reported mild preference for AEDE (f_EDE = 0.055^{+0.024}_{-0.047} at 68% CL) and the associated 2.6σ Hubble-tension reduction when DESI is added rest on the modeling choice that the DESI-CMB offset in ΛCDM is physical and best absorbed by AEDE. The abstract provides no details on priors for f_EDE or other AEDE parameters, nuisance parameters, or robustness tests against data splits or systematics; without these, it is difficult to evaluate whether the weak preference could be driven by unaccounted systematics in DESI reconstruction or CMB foregrounds instead.
minor comments (1)
  1. [Results] Ensure that all reported confidence levels (68% CL and 95% CL) and the exact data combinations are stated uniformly in the text, tables, and figure captions.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their positive evaluation of the significance of our work and for their detailed feedback. We address the single major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the reported mild preference for AEDE (f_EDE = 0.055^{+0.024}_{-0.047} at 68% CL) and the associated 2.6σ Hubble-tension reduction when DESI is added rest on the modeling choice that the DESI-CMB offset in ΛCDM is physical and best absorbed by AEDE. The abstract provides no details on priors for f_EDE or other AEDE parameters, nuisance parameters, or robustness tests against data splits or systematics; without these, it is difficult to evaluate whether the weak preference could be driven by unaccounted systematics in DESI reconstruction or CMB foregrounds instead.

    Authors: We thank the referee for this observation. The abstract already states that the parameter shift upon including DESI is a manifestation of the existing DESI-CMB discrepancy in ΛCDM, rather than claiming AEDE as the unique physical resolution. The model is presented as one that can accommodate the offset, yielding the reported mild preference and tension reduction. Full details on the AEDE parameter priors (flat prior on f_EDE from 0 to 0.3, following standard practice), other AEDE parameters, nuisance parameters in the CMB and BAO likelihoods, and robustness tests across data splits and systematics checks are provided in Sections 2–5 of the manuscript. To improve accessibility, we will revise the abstract to include a brief statement on the f_EDE prior range. revision: yes

Circularity Check

0 steps flagged

No significant circularity in direct data-driven constraints on AEDE

full rationale

The paper reports Bayesian posterior constraints on AEDE parameters (f_EDE, etc.) obtained by fitting the model directly to external CMB (SPT, ACT, Planck) and BAO (DESI) datasets. The quoted results, including f_EDE = 0.055^{+0.024}_{-0.047} and the 2.6σ Hubble tension reduction, are standard outputs of likelihood sampling on independent observations. No internal equation derives a quantity that is then renamed or refit as a prediction; no self-citation chain supplies a uniqueness theorem or ansatz that the present analysis depends upon; and the abstract explicitly frames the parameter shift as a consequence of the known DESI-CMB offset in ΛCDM rather than an internal construction. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 1 invented entities

The central results rest on standard cosmological parameter estimation applied to the AEDE model; limited information is available from the abstract alone.

free parameters (1)
  • f_EDE
    Fractional energy density contribution of the axion field at early times, directly constrained by the data fits.
axioms (1)
  • domain assumption Standard flat ΛCDM background cosmology modified by an early axion field component
    Invoked throughout the parameter estimation to compute theoretical power spectra and BAO scales.
invented entities (1)
  • Axion early dark energy field no independent evidence
    purpose: To provide additional early-universe energy density that alters the sound horizon and eases the Hubble tension
    Postulated model ingredient without independent detection or falsifiable signature outside the cosmological fit.

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