Atomic Dark Matter, Interacting Dark Radiation, and the Hubble Tension

Can Kilic; Gustavo Marques-Tavares; Ina Flood; Manuel A. Buen-Abad; Taewook Youn; Zackaria Chacko

Atomic Dark Matter, Interacting Dark Radiation, and the Hubble Tension

T0 review · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read nuADaM, a model of atomic dark matter plus self-interacting dark radiation, improves cosmological fits and raises the inferred Hubble constant to about 72.6 km/s/Mpc.

desk verdict A genuinely new dark-sector model with a real but conditional fit improvement, held back mainly by an unspecified post-BBN DR production mechanism. read the letter →

arxiv 2411.08097 v1 pith:ZV2QJPDJ submitted 2024-11-12 hep-ph astro-ph.CO

Manuel A. Buen-Abad , Zackaria Chacko , Ina Flood , Can Kilic , Gustavo Marques-Tavares , Taewook Youn This is my paper · ORCID

classification hep-phastro-ph.CO

keywords darkinteractingmattersubcomponentatomicmodelconventionaldata

topics The Hubble Tension

open problems The Hubble Tension

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

Most of the universe's matter is thought to be cold dark matter (CDM), which interacts only through gravity. Some models add a small fraction of 'atomic dark matter' that can feel a dark version of electromagnetism, and a bath of 'dark radiation' that interacts with itself. A known problem is that simple dark radiation solutions to the Hubble tension are disfavored by CMB data because they change the damping of acoustic peaks. This paper proposes a specific combination: a small subcomponent of dark matter formed of dark protons and dark electrons, coupled to self-interacting dark radiation. Before the CMB forms, this component behaves like a fluid with sound waves. Around the time of recombination, dark atoms form and decouple from the radiation, so that short-wavelength CMB modes that entered the horizon before decoupling feel different physics than longer modes. This step-like effect allows more dark radiation, which increases the inferred expansion rate H0, without ruining the CMB fit. The authors implement the model in a modified Boltzmann solver and run MCMC fits to Planck, BAO, supernova and full-shape clustering data, with and without the SH0ES H0 prior. They find their model gives a better fit than LCDM, especially when SH0ES is included, with H0 = 72.6 km/s/Mpc at the best fit. The model leaves some ingredients unspecified, such as how the dark radiation is created after BBN, and it does not resolve the Lyman-alpha forest tension.

Extended reading notes

Core claim

We show that this model admits a fit to the available cosmological data that is significantly better than both ΛCDM and conventional ADM. (Abstract) If true, nuADaM provides a viable dark-sector explanation of the Hubble tension, with H0 rising from about 68 to 72.6 km/s/Mpc at its best fit to Planck+BAO+Pantheon+SH0ES, without degrading CMB and full-shape clustering fits by more than O(1) in chi-squared.

Load-bearing premise

The paper assumes the dark radiation is populated only after Big Bang nucleosynthesis, via an unspecified dark-sector process that deposits energy into the DR after BBN concludes (Sec. 4, Footnote 8; Sec. 1). The large fitted values of ΔNeff (about 0.9) would otherwise violate BBN helium abundance constraints. If no such production mechanism exists, the model loses its ability to raise H0 and the claimed fit improvement disappears.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

The new thing here is genuine: nuADaM keeps the dark radiation self-interacting after dark recombination, which changes dark recombination to Case A and, more importantly, keeps the DR fluid-like at late times. That is a real difference from conventional ADM, and the paper shows it matters—nuADaM fits the DH dataset noticeably better than ADM while H0 lands near 72.6. The comparison is fair, and the authors' honesty about what they did not include (Lyman-alpha, full non-Gaussian posteriors) earns respect. The code modifications to CLASS and HyRec are real work, and the qualitative checks against Lyman-alpha and S8 are thoughtful.

The soft spots are in proportion. The biggest is the post-BBN DR population: the model as written has no coupling to the SM, and the analysis sets ΔNeff=0 during BBN by hand. The authors cite a generic possibility and leave the mechanism unspecified. That is not fatal—lots of dark-sector papers do this—but it is load-bearing, because absent such a mechanism the best-fit ΔNeff≈0.9 violates the helium bound. The paper says this, but it means the central claim is conditional on a microphysical story that does not yet exist. The H0 value is also a fit result, not a prediction, but that is standard for these analyses.

Other concerns are minor. The posteriors with full-shape data are multimodal, and the paper says so; the recombination treatment omits some heating terms, but the authors argue those are subdominant. The Lyman-alpha exclusion is well-motivated—the DAO make the standard likelihoods inapplicable—but it does leave a gap in the evidence.

If I were refereeing this, I would recommend publication after the production mechanism is addressed, or at least after the authors sharpen the claim to acknowledge that the model is a proof of principle. The paper is worth a serious referee; it is a credible step in a crowded field and the comparison with ADM is useful. I would cite it if I worked on interacting dark sectors, and I would bring it to reading group.

Assumptions & free parameters 6 free parameters · 6 assumptions · 5 invented entities

The central claim rests on six model parameters, three of which are fitted to the data and three fixed by hand. The key physical ingredients (dark atoms and self-interacting DR) are new entities without independent experimental evidence. Several axioms, including post-BBN DR production and Case A recombination, are assumed rather than derived.

free parameters (6)

Delta Neff = 0.90 (best fit to DH)
Energy density of self-interacting dark radiation relative to one neutrino species. Scanned in MCMC; the best fit requires non-zero values to raise H0.
fadm = 3.9% (best fit to DH)
Fraction of dark matter in the atomic subcomponent. Scanned in MCMC; best fit favors a few percent.
log10(me'/mp') = -3.7 (best fit to DH)
Log of dark electron to dark proton mass ratio; sets the dark recombination and decoupling redshifts. Scanned in MCMC.
alpha' (dark fine structure constant) = 10^-2 (fixed)
Fixed by hand because it is degenerate with mp' and Nf; controls binding energy and Thomson rates.
mp' (dark proton mass) = 1 GeV (fixed)
Fixed by hand; degenerate with other parameters in the cosmological fit.
Nf (number of dark neutrino flavors) = 3 (fixed)
Fixed by hand; affects DR degrees of freedom and scattering rates.

assumptions (6)

standard math FLRW cosmology and standard perturbation theory
Used throughout; CLASS implements these equations.
ad hoc to paper The dark radiation is populated after BBN by an unspecified mechanism
Stated in Sec. 4, Footnote 8; required for large Delta Neff without BBN constraints.
domain assumption Dark recombination is Case A (direct ground-state recombination) throughout
Sec. 3.1.3; the paper assumes this for the parameter space of interest, arguing it is realized for 10^-6 < epsilon < 10^-8 and 1 > alpha_X > 10^-2.
domain assumption The DR remains a perfect fluid at all relevant times
Sec. 3.1.1 and perturbation equations in Sec. 3.2 require vanishing higher moments; enforced by strong self-interactions.
domain assumption The perturbation equations from Refs. [34,69,70,71] apply to nuADaM
Sec. 3.2 uses the standard equations for atomic dark matter and DR, including Rayleigh and photo-ionization drag terms.
domain assumption Halofit is a valid nonlinear correction for nuADaM power spectra
Sec. 4 states Halofit makes a minute difference for similar interacting models, citing Ref. [65]; not validated for nuADaM itself.

invented entities (5)

Dark proton p'
purpose: Heavy fermion that forms dark hydrogen atoms
No direct detection; affects cosmological observables only through fadm and recombination.
Dark electron e'
purpose: Light fermion that controls dark recombination and Thomson scattering
Same; mass ratio sets decoupling epoch.
Dark photon A'
purpose: U(1) gauge boson mediating interactions between dark plasma and DR
No direct detection; its interactions set the decoupling rate.
Dark neutrinos nu'_j
purpose: Massless fermions that form the self-interacting dark radiation
No direct detection; only cosmological effects via Delta Neff.
Gauge boson X
purpose: U(1) gauge boson that keeps dark neutrinos self-interacting
No direct detection; required for fluid-like DR.

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Cite this review

Pith. "Pith review of Atomic Dark Matter, Interacting Dark Radiation, and the Hubble Tension." pith.science (2026). https://pith.science/paper/ZV2QJPDJ

@misc{pith2026241108097,
  author       = {Pith},
  title        = {Pith review of: Atomic Dark Matter, Interacting Dark Radiation, and the Hubble Tension},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZV2QJPDJ}},
  note         = {Machine review of arXiv:2411.08097}
}

abstract

We present a new class of interacting dark sector models that can address the Hubble tension. Interacting dark radiation (DR) has previously been put forward as a solution to the problem, but this proposal is disfavored by the high-$\ell$ cosmic microwave background (CMB) data. We modify this basic framework by introducing a subcomponent of dark matter (DM) that interacts strongly with the DR, so that together they constitute a tightly coupled fluid at early times. We show that if this subcomponent decouples from the interacting DR during the CMB epoch, the $\ell$ modes of the CMB that entered the horizon before decoupling are impacted differently from those that entered after, allowing a solution to the problem. We present a model that realizes this framework, which we dub "New Atomic Dark Matter", or nuADaM, in which the interacting dark matter (iDM) subcomponent is composed of dark atoms, and dark "neutrinos" with long-range interactions contribute to the DR, hence the name of the model. This iDM subcomponent is acoustic at early times but decouples from the DR following dark recombination. In contrast to conventional atomic dark matter (ADM) models, the dark photon is part of a richer DR sector, which ensures that it continues to be self-interacting even after recombination. We show that this model admits a fit to the available cosmological data that is significantly better than both $\Lambda$CDM and conventional ADM.

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Forward citations

Cited by 1 Pith paper

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

Hubble tension: a short review of theoretical explanations
astro-ph.CO 2026-07 accept novelty 4.0 of 10

A comprehensive review finds no theoretical Hubble-tension solution yet passes all consistency tests; new early-dark-energy chains reach high H0 only when the SH0ES calibration is added.

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