Sensitivity of Next-Generation CMB Surveys to Neutrinos and Other Light Relics

Anto I. Lonappan; Benjamin Wallisch; Carlo Baccigalupi; Christian L. Reichardt; Cynthia Trendafilova; Daniel Green; Daniel Grin; Edoardo Altamura; Emmanuel Schaan; Francis-Yan Cyr-Racine

REVIEW 2 major objections 3 minor 300 references

Sensitivity of Next-Generation CMB Surveys to Neutrinos and Other Light Relics

T0 review · 2 major / 3 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read The paper forecasts that a CMB-S4-scale survey can measure the effective number of relativistic species with $\sigma(N_\mathrm{eff}) = 0.029$, meeting the original science target of $0.030$, and that a cosmic-variance-limited successor…

desk verdict A careful, well-documented CMB-S4 Neff forecast with a public pipeline; the headline 0.029 meets the target only narrowly, so the foreground-model caveats matter more than usual, but this deserves a serious referee. read the letter →

arxiv 2608.07453 v1 pith:6V7PTYL7 submitted 2026-08-07 astro-ph.CO astro-ph.IMhep-phhep-th

Cynthia Trendafilova , Srinivasan Raghunathan , Benjamin Wallisch , Joel Meyers , Kevork N. Abazajian , Edoardo Altamura , Carlo Baccigalupi , Kimberly K. Boddy

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Thejs Brinckmann Yuji Chinone Gabriele Coppi Francis-Yan Cyr-Racine Jacques Delabrouille Katherine Freese Helena García Escudero Martina Gerbino Shamik Ghosh Vera Gluscevic Daniel Green Daniel Grin Kevin M. Huffenberger Mudit Jain Lloyd Knox Anto I. Lonappan Marilena Loverde Philip Lubin Gabriele Montefalcone Valentine Novosad Marco Raveri Christian L. Reichardt Sayan Saha Murali M. Saravanan Emmanuel Schaan Sara M. Simon Julien Tang Scott Watson (CMB-S4 Collaboration)

This is my paper · ORCID

classification astro-ph.COastro-ph.IMhep-phhep-th

keywords cosmicmicrowavebackgroundeffectivenumberofrelativisticspeciesNefflightthermalrelicsneutrinocosmologyFisher-matrixforecastsinternallinearcombinationdelensingCMBsurveydesign

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

The paper forecasts how precisely next-generation ground-based cosmic-microwave-background surveys could measure $N_\mathrm{eff}$, the effective number of relativistic species, which encodes the radiation content of the early universe beyond photons. Its central result is that the CMB-S4 two-site conceptual design, a wide Chilean survey combined with an ultra-deep South Pole patch, reaches $\sigma(N_\mathrm{eff}) = 0.029$ over seven years, meeting the project's original science target of $\sigma(N_\mathrm{eff}) = 0.030$, while the redesigned Chile-only configuration (a CMB-S4 hybrid LAT plus a Simons-Observatory-like telescope) reaches the same precision after nine years. A cosmic-variance-limited survey over the same multipole range would reach $\sigma(N_\mathrm{eff}) \approx 0.0073$, a factor of three to four better, showing how much primary-CMB information remains untapped. If these numbers hold, a CMB-S4-scale survey would for the first time be sensitive to any thermal relic of spin $\geq 1/2$ that ever equilibrated with the Standard Model, down to $\Delta N_\mathrm{eff} \approx 0.047$ for a Weyl fermion, and would test the physics of neutrino decoupling at the $1.5\sigma$ level.

What carries the argument

The load-bearing object is the DRAFT (Dark Radiation Anisotropy Flowdown Team) pipeline, an end-to-end forecasting tool that turns an experimental specification into a projected parameter error bar. It assembles a multi-frequency covariance from map-based PySM 3 galactic dust and synchrotron simulations plus SPT-calibrated templates for the thermal and kinematic Sunyaev-Zel'dovich effects, cosmic infrared background, and radio galaxies, applies the Planck GAL090 galactic mask, extracts the CMB with a minimum-variance internal linear combination (ILC), computes iteratively delensed TT/TE/EE spectra with CLASS delens, and feeds them into a Fisher-matrix calculation via FisherLens. The post-ILC residual spectra act as the effective noise entering the Gaussian, diagonal-in-multipole covariance, and the final $\sigma(N_\mathrm{eff})$ is read from the inverse Fisher matrix. The ILC step is where the paper's central optimism lives: minimum-variance ILC assumes the foreground spectral shapes are exactly known.

What would settle it

Rerun the DRAFT pipeline for the two-site conceptual design with spatially varying dust and synchrotron spectral indices, or with the measured tSZ-CIB correlation included, and check whether $\sigma(N_\mathrm{eff})$ rises above 0.030; likewise, the authors' own companion systematic-bias study, flagged as in preparation, settles the question if it shows foreground-induced biases at or above $\sigma(N_\mathrm{eff}) \approx 0.03$.

Watch

Extended reading notes

Core claim

The paper's claim is a sensitivity projection: with the DRAFT forecasting pipeline, the CMB-S4 two-site conceptual design achieves $\sigma(N_\mathrm{eff}) = 0.029$ in its nominal seven years, meeting the original CMB-S4 science target of $\sigma(N_\mathrm{eff}) = 0.030$, and the Chile-only revised configuration, jointly analyzing the CMB-S4 hybrid LAT with an SO-like wide survey over $f_\mathrm{sky} \approx 0.62$, reaches $\sigma(N_\mathrm{eff}) = 0.030$ after roughly nine years. The South-Pole-only alternative, with 20% of the sky after masking, falls about 22% short of the target at comparable cost, demonstrating that sky coverage rather than depth drives $N_\mathrm{eff}$ sensitivity because the information is spread across many acoustic peaks in the damping tail. The authors also show that polarization carries most of the small-scale constraining power, that the constraint saturates by $\ell_\mathrm{max} \approx 3750$ for the realistic survey, and that marginalizing over the primordial helium abundance $Y_p$ degrades $\sigma(N_\mathrm{eff})$ by a factor of 2.5, a degeneracy partially broken by the free-streaming neutrino phase shift.

Load-bearing premise

The forecasts assume the adopted foreground model is accurate and that the minimum-variance ILC knows the foreground shapes exactly; if real foregrounds deviate from the PySM 'model 0' templates and the SPT-based extragalactic parameterization, the projected $\sigma(N_\mathrm{eff})$ values are underestimated.

Editorial extensions

If this is right

At $\sigma(N_\mathrm{eff}) = 0.030$, the survey would detect or exclude a Weyl-fermion thermal relic at $1.6\sigma$ and a massless vector boson at $1.8\sigma$; a cosmic-variance-limited survey near $\sigma(N_\mathrm{eff}) \approx 0.01$ would reach almost $3\sigma$ for the lightest scalar, about $5\sigma$ for a Weyl fermion, and more than $5\sigma$ for a vector boson.
Because the $N_\mathrm{eff}$ information saturates by $\ell_\mathrm{max} \approx 3750$ for the realistic survey and lives mostly in E-mode polarization, the headline precision is robust to cutting small-scale temperature data, making the forecast resilient against many temperature systematics.
Marginalizing over the primordial helium abundance raises $\sigma(N_\mathrm{eff})$ from 0.029 to 0.072 for the conceptual design, so claims about beyond-Standard-Model physics at the 0.03 level hold only under the standard BBN consistency relation between $Y_p$, $\omega_b$, and $N_\mathrm{eff}$.
The gap between the CMB-S4-level forecasts and the cosmic-variance floor of $\sigma(N_\mathrm{eff}) = 0.0073$ quantifies the primary-CMB information still accessible to future full-sky or low-foreground missions.
The same observations would tighten constraints on the neutrino free-streaming phase shift, raising the lower bound on the free-streaming fraction of the radiation sector from about 82% today to above 96% at CMB-S4 precision.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

My reading: the headline numbers are statistical floors, not end-to-end systematics budgets; the paper's own caveats imply the real sensitivity will be set by how well foreground templates are validated, so an early empirical check is to compare DRAFT's post-ILC residuals against actual SO and SPT-3G small-scale polarization data.
The sky-coverage-over-depth result suggests that pushing below $\sigma(N_\mathrm{eff}) \approx 0.02$ naturally points to full-sky space surveys or northern-hemisphere wide patches, a direction the authors note but do not quantify, and the released machinery makes this a direct rescaling exercise.
The $\Delta N_\mathrm{eff} = 0.027$ scalar threshold is only about $3\sigma$ even at the cosmic-variance floor, implying that conclusively ruling out the lightest thermal scalar will require combining primary-CMB constraints with large-scale-structure or BBN information rather than CMB anisotropies alone.
If the $N_\mathrm{eff} \approx 2.8$ central value favored by current ACT+SPT+Planck data persists, the same forecasts imply a deviation well past $5\sigma$ at CMB-S4 precision, turning what is framed as a design-forecast paper into a discovery template for non-standard radiation content.

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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 useful new content here is concrete: which CMB-S4-style configuration reaches sigma(Neff)=0.030, how long it takes, and how far a cosmic-variance-limited survey sits below that. The Chile-only revised configuration reaching 0.030 after nine years and the CVL floor of 0.0073 are genuinely new numbers. The method is standard Fisher plus ILC plus delensing, but the implementation is careful: it checks the Gaussian likelihood assumption with DALI, uses established codes, and ships the DRAFT pipeline and precomputed residual spectra as public products. That is real, reproducible work and should count as such.

The central forecast is plausible but not robust to its own stated assumptions. The paper says in Section 3.1 that the foreground model is taken to be accurate, and in Section 3.4 that the minimum-variance ILC is somewhat optimistic because foreground shapes are assumed known. Since 0.029 sits only about 3 percent below the 0.030 target, a modest degradation in foreground residuals or an unmodeled bias from spatially varying dust SEDs could push the design past target. The stress-test note is right about this. It is not fatal: Neff constraints are driven mostly by TE and EE, where polarized foregrounds are subdominant, and the paper defends that with reference to prior ILC results. But the quantitative bias assessment is deferred to the unpublished companion paper [72], so the headline number should be read as the statistical sensitivity under exact foreground-shape knowledge, not as a guaranteed outcome.

Minor soft spots: the South-Pole-only noise model is a simple rescaling and the authors admit it; dropping patches 3 and 4 of the hybrid survey is reasonable but deserves a robustness check; and the Yp-degeneracy material is useful but secondary. The citation pattern is appropriate, heavy on CMB-S4 documents and SPT/Planck foreground papers, with nothing inflated. I also checked for circularity: no parameter is fitted to the 0.030 target; the forecast follows from the pipeline.

This paper is for CMB experiment planners, forecasters, and neutrino phenomenologists. It deserves a serious referee. I would send it to peer review, ask the referee to scrutinize the Chile-only timeline and the foreground-residual treatment, and suggest the authors soften the abstract until the companion systematic-bias study is available. As it stands, the paper is an honest and useful design reference, not a guaranteed prediction.

Referee Report

2 major / 3 minor

Summary. This paper presents Fisher-matrix forecasts of the sensitivity to the effective number of relativistic species, N_eff, for several CMB-S4 survey configurations considered during the project's design phase. The forecasting pipeline, implemented in the publicly released DRAFT tool, combines map-based Galactic foreground simulations and template-based extragalactic foregrounds, minimum-variance internal linear combination component separation, iterative delensing with CLASS delens, and a Gaussian Fisher covariance. The main quantitative results are that the two-site conceptual design reaches sigma(N_eff)=0.029 over seven years, thereby meeting the original CMB-S4 target of 0.030, the Chile-only revised configuration reaches 0.030 after nine years of combined CMB-S4 and SO-like operations, a South-Pole-only alternative achieves 0.037, and a cosmic-variance-limited survey over the same multipole range gives sigma(N_eff)=0.0073. The paper also discusses the implications of these sensitivities for thermal relics, radiation-sector properties, BBN, and other early-universe physics.

Significance. The forecasts are directly relevant to the planning of current and future ground-based CMB experiments and to the interpretation of their N_eff science goals. The paper has several concrete strengths: the DRAFT tool is publicly released; the pipeline uses established codes (CLASS delens, FisherLens) and validates the Gaussian Fisher assumption with DALI for the fiducial cosmology; intermediate products such as post-ILC residual spectra are made available; and the physics discussion in Section 5 is broad and well referenced. The central threshold claim, however, rests on optimistic or idealized assumptions that are acknowledged in the text but not quantitatively bounded, and the margin by which the conceptual design meets the science target is only a few percent. If the headline claim is to be used for design decisions, the robustness of sigma(N_eff)=0.029 to foreground-model uncertainty and to SO goal-versus-baseline noise should be demonstrated or the claim should be explicitly conditioned on those assumptions.

major comments (2)

[§3.1, §3.4, Table 6] The headline claim that the two-site conceptual design meets the CMB-S4 target with sigma(N_eff)=0.029 is computed from post-ILC residual spectra obtained under the assumption that the adopted foreground model is exactly correct. Section 3.1 states this explicitly, and Section 3.4 concedes that the MV-ILC is 'somewhat optimistic because it assumes that the shapes of the foreground signals are exactly known, which can lead to biased estimates of cosmological parameters.' Because 0.029 is only about 3% below the 0.030 target, even a modest increase in residual foreground power or a small SED mis-specification bias could push the forecast above the threshold. The argument that N_eff constraints are driven by TE and EE, where foregrounds are subdominant, addresses residual variance but does not quantify bias from mis-specified SED shapes in polarization. The paper does not provide this robustness quantification, despite noting that FisherLens includes an extended-Fisher bias estimator, and defers the analysis to the unpublished companion paper [72]. The manuscript should include a quantitative sensitivity test (for example, rescaling foreground amplitudes, varying dust and synchrotron SED parameters, or using a constrained ILC) or should explicitly frame the headline as conditional on the foreground model and remove the unqualified 'meets the target' language.
[§2.4, Table 6] The forecast that the Chile-only revised configuration reaches sigma(N_eff)=0.030 after nine years assumes that the SO-like large-aperture telescope reaches its 'goal' noise depth rather than its more conservative 'baseline' target, as stated in Section 2.4. No forecast using the baseline depth is presented, and no sensitivity of sigma(N_eff) to this assumption is given. Since the revised configuration reaches the threshold only after a long combined observing period, and the SO-like LAT contributes a substantial fraction of the sky area and depth, the goal-versus-baseline choice is material to the revised-configuration claim. The authors should present the baseline-depth result or quantitatively demonstrate that the difference is negligible.

minor comments (3)

[Abstract, §5, Table 7] The abstract and several discussion sections quote sigma(N_eff)=0.030 as the experiment's sensitivity without recalling that this holds when the primordial helium abundance Y_p is fixed by its BBN-consistent relation to omega_b and N_eff; Table 7 shows that marginalizing over Y_p degrades the conceptual-design constraint to 0.072. This model assumption should be restated wherever the headline sensitivity is quoted.
[Figure 6 caption and §2.4] The figure caption states that the negative-time range [-4,0] years corresponds to calendar years 2029-2033 for a nominal 2033 CMB-S4 start, while the text of Section 2.4 says the SO-like LAT begins observing in 2028. This inconsistency should be reconciled.
[§4.3] The statement that reaching sigma(N_eff)=0.030 from the South Pole alone would require 'roughly nine CMB-S4 Ultra-deep-like LATs and observe f_sky=0.25 over a period of 20 years' is not derived in the text; either show the scaling argument behind this estimate or cite the analysis in which it was obtained.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the sigma(Neff) forecasts are computed from externally specified noise, sky fraction, and foreground models, with no parameter fitted to the 0.030 target.

full rationale

The derivation chain runs from survey specifications (noise, beams, noise knees from the CMB-S4 design report and SO forecasts), foreground models (PySM3 simulations and SPT-template parameters), and known LambdaCDM+Neff theory, through MV-ILC residuals, CLASS delens/FisherLens, and the Gaussian Fisher covariance (3.5). The target sigma(Neff)=0.030 is external to the pipeline; the paper explicitly states the forecasts 'assume the adopted model to be accurate and do not account for residual uncertainties in the foreground modeling itself' (Section 3.1) and that the MV-ILC choice is 'somewhat optimistic because it assumes that the shapes of the foreground signals are exactly known' (Section 3.4). These are explicit caveats and defer bias quantification to the companion paper [72]; they are correctness or robustness risks, not circular reductions. The light-relic thresholds of 0.027, 0.047, and 0.054 follow from Eq. (5.1) with Standard Model g*S(TF), not from the Fisher results. Self-citations to CLASS delens, FisherLens, and DRAFT are methodological code and implementation references, with external validation and comparison to current Planck, ACT, and SPT constraints; none of the load-bearing equations is defined in terms of the target result. No fitted input is renamed as a prediction, and no uniqueness theorem is imported to force a design choice. The central forecast therefore has independent content and is not circular.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The central forecasts depend on assumed noise and foreground specifications, the chosen fiducial cosmology, and the ILC and delensing assumptions. No new physical entities are introduced. The numbers are inputs from prior measurements or design documents, not fitted to the forecasted target.

free parameters (4)

Extragalactic foreground amplitudes at 150 GHz and ell=3000 (tSZ, kSZ, CIB Poisson, CIB clustered, radio) = 3.4, 3.0, 9.1, 3.4, 1.0 microK^2 respectively
Adopted from SPT best-fit parameterization in Section 3.1 and Table 4; these amplitudes set the ILC residuals and therefore the projected sensitivity.
Galactic foreground spectral parameters (dust temperature, dust emissivity index, synchrotron spectral index, TE… = 19.6 K, 1.53, -3.1, 0.35 for dust and 0 for synchrotron
Fixed from Planck observations and used in PySM-based galactic simulations in Section 3.1; not varied in the forecasts.
Fiducial cosmological parameters (omega_b, omega_c, theta_s, A_s, n_s, tau, N_eff) = 0.0222, 0.1197, 0.010409, 2.196e-9, 0.9655, 0.060, 3.044
Fiducial LambdaCDM+Neff model in Table 5; Fisher derivatives are evaluated at this point, so the projected uncertainties depend on these choices.
SO-like LAT goal noise depth versus baseline depth = Goal depth from Table 1 of reference [67]
The revised configuration forecast assumes the SO-like LAT reaches its goal depth rather than the conservative baseline (Section 2.4), which shortens the time to sigma=0.030.

assumptions (5)

domain assumption LambdaCDM + Neff with fixed sum of neutrino masses and BBN-consistent helium abundance is the correct fiducial cosmology.
Used in Section 3.3 and Table 5; if Neff and Sigma(m_nu) are correlated beyond the stated check, the forecast changes.
standard math Gaussian Fisher information and the Cramer-Rao bound are valid for the considered power spectra.
Fisher formalism in Section 3.3; verified for this cosmology with DALI in reference [114].
domain assumption The foreground templates and scaling laws are accurate, and unresolved sources are masked at S150=6 mJy.
Section 3.1; adopted from SPT and ACT measurements without propagating their uncertainties.
domain assumption Minimum-variance ILC with perfectly known foreground spectral shapes yields the computed residual spectra.
Sections 3.2 and 3.4; the paper calls this assumption somewhat optimistic.
domain assumption Iterative delensing with CLASS delens achieves the predicted lensing-reconstruction noise.
Section 3.3; delensing matters for the CMB-S4 forecasts and even more for the cosmic-variance-limited floor.

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Cite this review

Pith. "Pith review of Sensitivity of Next-Generation CMB Surveys to Neutrinos and Other Light Relics." pith.science (2026). https://pith.science/paper/6V7PTYL7

@misc{pith2026260807453,
  author       = {Pith},
  title        = {Pith review of: Sensitivity of Next-Generation CMB Surveys to Neutrinos and Other Light Relics},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6V7PTYL7}},
  note         = {Machine review of arXiv:2608.07453}
}

abstract

Neutrinos and other light relics leave characteristic imprints in the cosmic microwave background anisotropies, making their observation a sensitive probe of the particle content and thermal history of the early universe. The energy density in these relativistic species is parameterized by their effective number $N_\mathrm{eff}$. Measuring this parameter at the percent level, which is a long-standing science goal of CMB-S4 and other experiments, would test a wide range of well-motivated physics within and beyond the Standard Model of particle physics. In this paper, we present Fisher-matrix forecasts of the projected sensitivity to $N_\mathrm{eff}$ of several CMB-S4 survey configurations considered during its extensive design phase. The conceptual design reaches $\sigma(N_\mathrm{eff}) < 0.03$ over its seven-year observing period, while the revised configuration achieves the same precision over a longer timescale. We complement these results with a cosmic-variance-limited survey over the same multipole range to quantify the room for improvement accessible with additional instrumental, observational, and theoretical efforts. Finally, we discuss the broad implications of precise $N_\mathrm{eff}$ measurements for the radiation sector, big bang nucleosynthesis, light thermal relics, and other early-universe physics. The forecasts presented in this work are performed with the publicly released DRAFT (Dark Radiation Anisotropy Flowdown Team) tool. It provides an end-to-end pipeline from simulated foreground maps and component separation to delensing and projected sensitivities for any cosmological parameter, and it can be directly applied to other cosmic microwave background survey designs.

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Reference graph

Works this paper leans on

300 extracted references · 3 canonical work pages

[72]

Raghunathan, C

S. Raghunathan, C. Trendafilova, J. Meyers, B. Wallisch et al., in preparation
[1]

Snowmass Theory Frontier: Astrophysics and Cosmology

D. Green et al., “Snowmass Theory Frontier: Astrophysics and Cosmology”,arXiv:2209.06854 [hep-ph]

arXiv
[2]

Report of the Topical Group on Cosmic Frontier 5 Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before for Snowmass 2021

C. Chang et al., “Report of the Topical Group on Cosmic Frontier 5 Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before for Snowmass 2021”,arXiv:2209.08265 [hep-ex]

arXiv 2021
[3]

TASI Lectures on Cosmic Signals of Fundamental Physics

D. Green, “TASI Lectures on Cosmic Signals of Fundamental Physics”,PoSTASI2022(2024) 005, arXiv:2212.08685 [hep-ph]

arXiv 2024
[4]

Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics

D. Green et al., “Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics”, Bull. Am. Astron. Soc.51(2019) 159,arXiv:1903.04763 [astro-ph.CO]

arXiv 2019
[5]

Synergy between Cosmological and Laboratory Searches in Neutrino Physics

M. Gerbino et al., “Synergy between Cosmological and Laboratory Searches in Neutrino Physics”, Phys. Dark Univ.42(2023) 101333,arXiv:2203.07377 [hep-ph]

arXiv 2023
[6]

The Physics of Light Relics

C. Dvorkin et al., “The Physics of Light Relics”,arXiv:2203.07943 [hep-ph]

arXiv
[7]

Prospects and Limitations for Constraining Light Relics with Primordial Abundance Measurements

A. Lagu¨ e and J. Meyers, “Prospects and Limitations for Constraining Light Relics with Primordial Abundance Measurements”,Phys. Rev. D101(2020) 043509, arXiv:1908.05291 [astro-ph.CO]

arXiv 2020

Show all 300 references

[8]

Primordial Deuterium after LUNA: Concordances and Error Budget

O. Pisanti, G. Mangano, G. Miele, and P. Mazzella, “Primordial Deuterium after LUNA: Concordances and Error Budget”,JCAP04(2021) 020,arXiv:2011.11537 [astro-ph.CO]

2021 arXiv
[9]

The Impact of Newd(p,γ) 3He Rates on Big Bang Nucleosynthesis

T.-H. Yeh, K. Olive, and B. Fields, “The Impact of Newd(p,γ) 3He Rates on Big Bang Nucleosynthesis”,JCAP03(2021) 046,arXiv:2011.13874 [astro-ph.CO]

2021 arXiv
[10]

EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-Poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension

A. Matsumoto et al., “EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-Poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension”,Astrophys. J.941(2022) 167,arXiv:2203.09617 [astro-ph.CO]

2022 arXiv
[11]

Probing Physics beyond the Standard Model: Limits from BBN and the CMB Independently and Combined

T.-H. Yeh, J. Shelton, K. Olive, and B. Fields, “Probing Physics beyond the Standard Model: Limits from BBN and the CMB Independently and Combined”,JCAP10(2022) 046, arXiv:2207.13133 [astro-ph.CO]

2022 arXiv
[12]

EMPRESS. XV. A New Determination of the Primordial Helium Abundance Suggesting a Moderately LowY p Value

H. Yanagisawa et al., “EMPRESS. XV. A New Determination of the Primordial Helium Abundance Suggesting a Moderately LowY p Value”,Astrophys. J.1004(2026) 55,arXiv:2506.24050 [astro-ph.GA]

2026 arXiv
[13]

The LBTY p Project V: Cosmological Implications of a New Determination of Primordial 4He

T.-H. Yeh, K. Olive, B. Fields, E. Aver, R. Pogge, N. Rogers, E. Skillman, and M. Weller, “The LBTY p Project V: Cosmological Implications of a New Determination of Primordial 4He”, arXiv:2601.22239 [astro-ph.CO]
[14]

Precision Big Bang Nucleosynthesis with Improved Helium-4 Predictions

C. Pitrou, A. Coc, J.-P. Uzan, and E. Vangioni, “Precision Big Bang Nucleosynthesis with Improved Helium-4 Predictions”,Phys. Rept.754(2018) 1,arXiv:1801.08023 [astro-ph.CO]

2018 arXiv
[15]

Big Bang Nucleosynthesis and Neutrino Cosmology

E. Grohs, J. R. Bond, R. Cooke, G. Fuller, J. Meyers, and M. Paris, “Big Bang Nucleosynthesis and Neutrino Cosmology”,Bull. Am. Astron. Soc.51(2019) 412,arXiv:1903.09187 [astro-ph.CO]

2019 arXiv
[16]

Big Bang Nucleosynthesis after Planck

B. Fields, K. Olive, T.-H. Yeh, and C. Young, “Big Bang Nucleosynthesis after Planck”,JCAP03 (2020) 010,arXiv:1912.01132 [astro-ph.CO]

2020 arXiv
[17]

Big Bang Nucleosynthesis

E. Grohs and G. Fuller, “Big Bang Nucleosynthesis”,Handbook of Nuclear Physics(2022) 1, arXiv:2301.12299 [astro-ph.CO]

2022 arXiv
[18]

Big Bang Nucleosynthesis

R. Cooke, “Big Bang Nucleosynthesis”,Encyclopedia of Astrophysics5(2026) 159, arXiv:2409.06015 [astro-ph.CO]

2026 arXiv
[19]

Searching for Light Relics with Large-Scale Structure

D. Baumann, D. Green, and B. Wallisch, “Searching for Light Relics with Large-Scale Structure”, 52 JCAP08(2018) 029,arXiv:1712.08067 [astro-ph.CO]

2018 arXiv
[20]

Cosmology in the Era of Euclid and the Square Kilometre Array

T. Sprenger, M. Archidiacono, T. Brinckmann, S. Clesse, and J. Lesgourgues, “Cosmology in the Era of Euclid and the Square Kilometre Array”,JCAP02(2019) 047,arXiv:1801.08331 [astro-ph.CO]

2019 arXiv
[21]

Inflation and Early Dark Energy with a Stage-II Hydrogen Intensity Mapping Experiment

R. Ansari et al. (Cosmic Visions 21 cm Collaboration), “Inflation and Early Dark Energy with a Stage-II Hydrogen Intensity Mapping Experiment”,arXiv:1810.09572 [astro-ph.CO]

arXiv
[22]

First Constraint on the Neutrino-Induced Phase Shift in the Spectrum of Baryon Acoustic Oscillations

D. Baumann, F. Beutler, R. Flauger, D. Green, A. Slosar, M. Vargas-Maga˜ na, B. Wallisch, and C. Y` eche, “First Constraint on the Neutrino-Induced Phase Shift in the Spectrum of Baryon Acoustic Oscillations”,Nature Phys.15(2019) 465,arXiv:1803.10741 [astro-ph.CO]

2019 arXiv
[23]

Packed Ultra-wideband Mapping Array (PUMA): A Radio Telescope for Cosmology and Transients

A. Slosar et al. (PUMA Collaboration), “Packed Ultra-wideband Mapping Array (PUMA): A Radio Telescope for Cosmology and Transients”,Bull. Am. Astron. Soc.51(2019) 53, arXiv:1907.12559 [astro-ph.IM]

2019 arXiv
[24]

Cosmology at High Redshift – A Probe of Fundamental Physics

N. Sailer, E. Castorina, S. Ferraro, and M. White, “Cosmology at High Redshift – A Probe of Fundamental Physics”,JCAP12(2021) 049,arXiv:2106.09713 [astro-ph.CO]

2021 arXiv
[25]

Neutrino Properties with Ground-Based Millimeter-Wavelength Line Intensity Mapping

A. Moradinezhad Dizgah, G. Keating, K. Karkare, A. Crites, and S. Choudhury, “Neutrino Properties with Ground-Based Millimeter-Wavelength Line Intensity Mapping”,Astrophys. J.926 (2022) 137,arXiv:2110.00014 [astro-ph.CO]

2022 arXiv
[26]

Snowmass 2021 Cosmic Frontier White Paper: Cosmology with Millimeter-Wave Line Intensity Mapping

K. Karkare, A. Moradinezhad Dizgah, G. Keating, P. Breysse, and D. Chung, “Snowmass 2021 Cosmic Frontier White Paper: Cosmology with Millimeter-Wave Line Intensity Mapping”,arXiv:2203.07258 [astro-ph.CO]

2021 arXiv
[27]

Constraining Effective Neutrino Species with Bispectrum of Large-Scale Structures

Y. Shi, C. Heinrich, and O. Dor´ e, “Constraining Effective Neutrino Species with Bispectrum of Large-Scale Structures”,Phys. Rev. D108(2023) 023522,arXiv:2208.10560 [astro-ph.CO]

2023 arXiv
[28]

Probing Light Relics through Cosmic Dawn

N. Lee and S. Hotinli, “Probing Light Relics through Cosmic Dawn”,Phys. Rev. D109(2024) 043502,arXiv:2309.15119 [astro-ph.CO]

2024 arXiv
[29]

Euclid Preparation – LIV. Sensitivity to Neutrino Parameters

M. Archidiacono et al. (Euclid Collaboration), “Euclid Preparation – LIV. Sensitivity to Neutrino Parameters”,Astron. Astrophys.693(2025) A58,arXiv:2405.06047 [astro-ph.CO]

2025
[30]

Probing New Physics beyond ΛCDM with Large-Scale Structure

A. Moradinezhad Dizgah, “Probing New Physics beyond ΛCDM with Large-Scale Structure”, SciPost Phys. Lect. Notes116(2026) 1

2026
[31]

The DESI Experiment Part I: Science, Targeting, and Survey Design

A. Aghamousa et al. (DESI Collaboration), “The DESI Experiment Part I: Science, Targeting, and Survey Design”,arXiv:1611.00036 [astro-ph.IM]

arXiv
[32]

Euclid Preparation – I. The Euclid Wide Survey

R. Scaramella et al. (Euclid Collaboration), “Euclid Preparation – I. The Euclid Wide Survey”, Astron. Astrophys.662(2022) A112,arXiv:2108.01201 [astro-ph.CO]

2022 arXiv
[33]

MUltiplexed Survey Telescope: Perspectives for Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys

C. Zhao et al., “MUltiplexed Survey Telescope: Perspectives for Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys”,arXiv:2411.07970 [astro-ph.CO]

arXiv
[34]

A Spectroscopic Road Map for Cosmic Frontier: DESI, DESI-II, Stage-5

D. Schlegel et al. (DESI Collaboration), “A Spectroscopic Road Map for Cosmic Frontier: DESI, DESI-II, Stage-5”,arXiv:2209.03585 [astro-ph.CO]

arXiv
[35]

Lesgourgues, G

J. Lesgourgues, G. Mangano, G. Miele, and S. Pastor,Neutrino Cosmology, Cambridge University Press, 2013

2013
[36]

Neutrino Physics from the Cosmic Microwave Background and Large-Scale Structure

K. Abazajian et al., “Neutrino Physics from the Cosmic Microwave Background and Large-Scale Structure”,Astropart. Phys.63(2015) 66,arXiv:1309.5383 [astro-ph.CO]

2015 arXiv
[37]

Neutrino Physics from the Cosmic Microwave Background and 53 Large-Scale Structure

K. Abazajian and M. Kaplinghat, “Neutrino Physics from the Cosmic Microwave Background and 53 Large-Scale Structure”,Ann. Rev. Nucl. Part. Sci.66(2016) 401

2016
[38]

Dark Sectors 2016 Workshop: Community Report

J. Alexander et al., “Dark Sectors 2016 Workshop: Community Report”,arXiv:1608.08632 [hep-ph]

2016 arXiv
[39]

CMB-S4 Science Book, First Edition

K. Abazajian et al. (CMB-S4 Collaboration), “CMB-S4 Science Book, First Edition”, arXiv:1610.02743 [astro-ph.CO]

arXiv
[40]

Status of Neutrino Properties and Future Prospects – Cosmological and Astrophysical Constraints

M. Lattanzi and M. Gerbino, “Status of Neutrino Properties and Future Prospects – Cosmological and Astrophysical Constraints”,Front. in Phys.5(2018) 70,arXiv:1712.07109 [astro-ph.CO]

2018 arXiv
[41]

Wallisch,Cosmological Probes of Light Relics, PhD Thesis, University of Cambridge, 2018, arXiv:1810.02800 [astro-ph.CO]

B. Wallisch,Cosmological Probes of Light Relics, PhD Thesis, University of Cambridge, 2018, arXiv:1810.02800 [astro-ph.CO]

2018 arXiv
[42]

Early-Universe Model Building

P. Asadi et al., “Early-Universe Model Building”,arXiv:2203.06680 [hep-ph]

arXiv
[43]

Feebly-Interacting Particles: FIPs 2022 Workshop Report

C. Antel et al., “Feebly-Interacting Particles: FIPs 2022 Workshop Report”,Eur. Phys. J. C83 (2023) 1122,arXiv:2305.01715 [hep-ph]

2023 arXiv
[44]

How Massless Neutrinos Affect the Cosmic Microwave Background Damping Tail

Z. Hou, R. Keisler, L. Knox, M. Millea, and C. Reichardt, “How Massless Neutrinos Affect the Cosmic Microwave Background Damping Tail”,Phys. Rev. D87(2013) 083008, arXiv:1104.2333 [astro-ph.CO]

2013 arXiv
[45]

Neutrino Perturbations in CMB Anisotropy and Matter Clustering

S. Bashinsky and U. Seljak, “Neutrino Perturbations in CMB Anisotropy and Matter Clustering”, Phys. Rev. D69(2004) 083002,arXiv:astro-ph/0310198

2004 arXiv
[46]

First Detection of the Acoustic Oscillation Phase Shift Expected from the Cosmic Neutrino Background

B. Follin, L. Knox, M. Millea, and Z. Pan, “First Detection of the Acoustic Oscillation Phase Shift Expected from the Cosmic Neutrino Background”,Phys. Rev. Lett.115(2015) 091301, arXiv:1503.07863 [astro-ph.CO]

2015 arXiv
[47]

Phases of New Physics in the CMB

D. Baumann, D. Green, J. Meyers, and B. Wallisch, “Phases of New Physics in the CMB”,JCAP 01(2016) 007,arXiv:1508.06342 [astro-ph.CO]

2016 arXiv
[48]

Free-Streaming Neutrinos and Their Phase Shift in Current and Future CMB Power Spectra

G. Montefalcone, B. Wallisch, and K. Freese, “Free-Streaming Neutrinos and Their Phase Shift in Current and Future CMB Power Spectra”,JCAP08(2025) 051,arXiv:2501.13788 [astro-ph.CO]

2025
[49]

Directly Probing Neutrino Interactions through CMB Phase Shift Measurements

G. Montefalcone, S. Ghosh, K. Boddy, D. Ho, and Y. Tsai, “Directly Probing Neutrino Interactions through CMB Phase Shift Measurements”,Phys. Rev. D113(2026) 023540,arXiv:2509.20363 [astro-ph.CO]

2026
[50]

A Precision Calculation of Relic Neutrino Decoupling

K. Akita and M. Yamaguchi, “A Precision Calculation of Relic Neutrino Decoupling”,JCAP08 (2020) 012,arXiv:2005.07047 [hep-ph]

2020 arXiv
[51]

Neutrino Decoupling Including Flavor Oscillations and Primordial Nucleosynthesis

J. Froustey, C. Pitrou, and M. C. Volpe, “Neutrino Decoupling Including Flavor Oscillations and Primordial Nucleosynthesis”,JCAP12(2020) 015,arXiv:2008.01074 [hep-ph]

2020 arXiv
[52]

Towards a Precision Calculation ofN eff in the Standard Model II: Neutrino Decoupling in the Presence of Flavor Oscillations and Finite-Temperature QED

J. Bennett, G. Buldgen, P. de Salas, M. Drewes, S. Gariazzo, S. Pastor, and Y. Y. Y. Wong, “Towards a Precision Calculation ofN eff in the Standard Model II: Neutrino Decoupling in the Presence of Flavor Oscillations and Finite-Temperature QED”,JCAP04(2021) 073, arXiv:2012.027...

2021 arXiv
[53]

Neff in the Standard Model at NLO is 3.043

M. Cielo, M. Escudero, G. Mangano, and O. Pisanti, “ Neff in the Standard Model at NLO is 3.043”, Phys. Rev. D108(2023) L121301,arXiv:2306.05460 [hep-ph]

2023 arXiv
[54]

Towards a Precision Calculation of Neff in the Standard Model. Part III. Improved Estimate of NLO Corrections to the Collision Integral

M. Drewes, Y. Georis, M. Klasen, L. P. Wiggering, and Y. Y. Y. Wong, “Towards a Precision Calculation of Neff in the Standard Model. Part III. Improved Estimate of NLO Corrections to the Collision Integral”,JCAP06(2024) 032,arXiv:2402.18481 [hep-ph]. 54

2024 arXiv
[55]

Towards a Precision Calculation ofN eff in the Standard Model IV: Estimating the Impact of Positronium Formation

T. Binder, M. Drewes, Y. Georis, M. Klasen, G. Pierobon, and Y. Y. Y. Wong, “Towards a Precision Calculation ofN eff in the Standard Model IV: Estimating the Impact of Positronium Formation”,JCAP10(2025) 069,arXiv:2411.14091 [hep-ph]

2025
[56]

Precision Calculation of Neff with Neutrino Direct-Simulation Monte Carlo

O. Ihnatenko and M. Ovchynnikov, “Precision Calculation of Neff with Neutrino Direct-Simulation Monte Carlo”,Phys. Rev. D112(2025) 103543,arXiv:2508.08379 [hep-ph]

2025
[57]

Fast and Flexible Neutrino Decoupling. Part I. The Standard Model

M. Escudero, G. Jackson, M. Laine, and S. Sandner, “Fast and Flexible Neutrino Decoupling. Part I. The Standard Model”,JCAP02(2026) 046,arXiv:2511.04747 [hep-ph]

2026
[58]

Planck 2018 Results. VI. Cosmological Parameters

N. Aghanim et al. (Planck Collaboration), “Planck 2018 Results. VI. Cosmological Parameters”, Astron. Astrophys.641(2020) A6,arXiv:1807.06209 [astro-ph.CO]

2020 arXiv
[59]

The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models

E. Calabrese et al. (ACT Collaboration), “The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models”,JCAP11(2025) 063,arXiv:2503.14454 [astro-ph.CO]

2025 arXiv
[60]

SPT-3G D1: CMB Temperature and Polarization Power Spectra and Cosmology from 2019 and 2020 Observations of the SPT-3G Main Field

E. Camphuis et al. (SPT-3G Collaboration), “SPT-3G D1: CMB Temperature and Polarization Power Spectra and Cosmology from 2019 and 2020 Observations of the SPT-3G Main Field”,Phys. Rev. D113(2026) 083504,arXiv:2506.20707 [astro-ph.CO]

2026 arXiv
[61]

CMB Power Spectra and Cosmological Parameters from Planck PR4 with CamSpec

E. Rosenberg, S. Gratton, and G. Efstathiou, “CMB Power Spectra and Cosmological Parameters from Planck PR4 with CamSpec”,Mon. Not. Roy. Astron. Soc.517(2022) 4620, arXiv:2205.10869 [astro-ph.CO]

2022 arXiv
[62]

Cosmological Parameters Derived from the Final Planck Data Release (PR4)

M. Tristram et al., “Cosmological Parameters Derived from the Final Planck Data Release (PR4)”, Astron. Astrophys.682(2024) A37,arXiv:2309.10034 [astro-ph.CO]

2024 arXiv
[63]

Limits on the Cosmic Neutrino Background

M. Bauer and J. Shergold, “Limits on the Cosmic Neutrino Background”,JCAP01(2023) 003, arXiv:2207.12413 [hep-ph]

2023 arXiv
[64]

The Cosmic Neutrino Background

D. Scott, “The Cosmic Neutrino Background”,arXiv:2402.16243 [astro-ph.CO]

arXiv
[65]

Testing the ΛCDM Cosmological Model with Forthcoming Measurements of the Cosmic Microwave Background with SPT-3G

K. Prabhu et al. (SPT-3G Collaboration), “Testing the ΛCDM Cosmological Model with Forthcoming Measurements of the Cosmic Microwave Background with SPT-3G”,Astrophys. J.973 (2024) 4,arXiv:2403.17925 [astro-ph.CO]

2024 arXiv
[66]

The Simons Observatory: Science Goals and Forecasts

P. Ade et al. (Simons Observatory Collaboration), “The Simons Observatory: Science Goals and Forecasts”,JCAP02(2019) 056,arXiv:1808.07445 [astro-ph.CO]

2019 arXiv
[67]

The Simons Observatory: Science Goals and Forecasts for the Enhanced Large-Aperture Telescope

M. Abitbol et al. (Simons Observatory Collaboration), “The Simons Observatory: Science Goals and Forecasts for the Enhanced Large-Aperture Telescope”,JCAP08(2025) 034,arXiv:2503.00636 [astro-ph.IM]

2025 arXiv
[68]

CMB-S4 Science Case, Reference Design, and Project Plan

K. Abazajian et al. (CMB-S4 Collaboration), “CMB-S4 Science Case, Reference Design, and Project Plan”,arXiv:1907.04473 [astro-ph.IM]

1907 arXiv
[69]

Snowmass 2021 CMB-S4 White Paper

K. Abazajian et al. (CMB-S4 Collaboration), “Snowmass 2021 CMB-S4 White Paper”, arXiv:2203.08024 [astro-ph.CO]

2021 arXiv
[70]

CMB-S4 Design Report 2023

K. Abazajian et al. (CMB-S4 Collaboration), “CMB-S4 Design Report 2023”, CMBS4-doc-716-v6 (2023)

2023
[71]

Snowmass 2021 Cosmic Frontier: Cosmic Microwave Background Measurements White Paper

C. Chang et al., “Snowmass 2021 Cosmic Frontier: Cosmic Microwave Background Measurements White Paper”,arXiv:2203.07638 [astro-ph.CO]

2021
[73]

Towards a Cosmological Neutrino Mass Detection

R. Allison, P. Caucal, E. Calabrese, J. Dunkley, and T. Louis, “Towards a Cosmological Neutrino Mass Detection”,Phys. Rev. D92(2015) 123535,arXiv:1509.07471 [astro-ph.CO]. 55

2015 arXiv
[74]

Optimization of Multi-Resolution Observation Strategies for CMB Experiments

S. Simon, J. Delabrouille, J. Carron, R. Keskitalo, D. Barron and S. Ghosh, “Optimization of Multi-Resolution Observation Strategies for CMB Experiments”, in preparation
[75]

Planck 2015 Results. X. Diffuse Component Separation: Foreground Maps

R. Adam et al. (Planck Collaboration), “Planck 2015 Results. X. Diffuse Component Separation: Foreground Maps”,Astron. Astrophys.594(2016) A10,arXiv:1502.01588 [astro-ph.CO]

2016 arXiv
[76]

Planck 2015 Results. I. Overview of Products and Scientific Results

R. Adam et al. (Planck Collaboration), “Planck 2015 Results. I. Overview of Products and Scientific Results”,Astron. Astrophys.594(2016) A1,arXiv:1502.01582 [astro-ph.CO]

2016 arXiv
[77]

CMB-S4 Study to Support the Alternatives Analysis and Selection

K. Abazajian et al. ( CMB-S4 Collaboration), “CMB-S4 Study to Support the Alternatives Analysis and Selection”, CMBS4-doc-1004-v3 (2023)

2023
[78]

CMB-S4: Forecasting Constraints on Primordial Gravitational Waves

K. Abazajian et al. (CMB-S4 Collaboration), “CMB-S4: Forecasting Constraints on Primordial Gravitational Waves”,Astrophys. J.926(2022) 54,arXiv:2008.12619 [astro-ph.CO]

2022 arXiv
[79]

Revised CMB-S4 Project Plan

K. Abazajian et al. ( CMB-S4 Collaboration), “Revised CMB-S4 Project Plan”, CMBS4-doc-1095-v1 (2025)

2025
[80]

Dunkley, private communication (2026)

J. Dunkley, private communication (2026)

2026
[81]

Map-Based Simulations for CMB-S4 (Design Tool Run)

A. Zonca et al. ( CMB-S4 Collaboration), “Map-Based Simulations for CMB-S4 (Design Tool Run)”, https:/ /github.com/CMB-S4/s4mapbasedsims/tree/main/202102design tool run (2021)

2021
[82]

The Python Sky Model: Software for Simulating the Galactic Microwave Sky

B. Thorne, J. Dunkley, D. Alonso, and S. Naess, “The Python Sky Model: Software for Simulating the Galactic Microwave Sky”,Mon. Not. Roy. Astron. Soc.469(2017) 2821,arXiv:1608.02841 [astro-ph.CO]

2017 arXiv
[83]

The Python Sky Model 3 Software

A. Zonca, B. Thorne, N. Krachmalnicoff, and J. Borrill, “The Python Sky Model 3 Software”,J. Open Source Softw.6(2021) 3783,arXiv:2108.01444 [astro-ph.IM]

2021 arXiv
[84]

Documentation of the PySM Simulations for the Simons Observatory

A. Zonca et al., “Documentation of the PySM Simulations for the Simons Observatory”, https:/ /so-pysm-models.readthedocs.io/en/latest/index.html (2022)

2022
[85]

Planck 2018 Results. XI. Polarized Dust Foregrounds

Y. Akrami et al. (Planck Collaboration), “Planck 2018 Results. XI. Polarized Dust Foregrounds”, Astron. Astrophys.641(2020) A11,arXiv:1801.04945 [astro-ph.GA]

2020 arXiv
[86]

Constraining Cluster Virialization Mechanism and Cosmology using Thermal-SZ-Selected Clusters from Future CMB Surveys

S. Raghunathan, N. Whitehorn, M. Alvarez, H. Aung, N. Battaglia, G. Holder, D. Nagai, E. Pierpaoli, C. Reichardt, and J. Vieira, “Constraining Cluster Virialization Mechanism and Cosmology using Thermal-SZ-Selected Clusters from Future CMB Surveys”,Astrophys. J.926 (2022) 172,...

2022 arXiv
[87]

A Measurement of Secondary Cosmic Microwave Background Anisotropies from the 2500 deg2 SPT-SZ Survey

E. George et al., “A Measurement of Secondary Cosmic Microwave Background Anisotropies from the 2500 deg2 SPT-SZ Survey”,Astrophys. J.799(2015) 177,arXiv:1408.3161 [astro-ph.CO]

2015 arXiv
[88]

An Improved Measurement of the Secondary Cosmic Microwave Background Anisotropies from the SPT-SZ + SPTpol Surveys

C. Reichardt et al. (SPT Collaboration), “An Improved Measurement of the Secondary Cosmic Microwave Background Anisotropies from the SPT-SZ + SPTpol Surveys”,Astrophys. J.908 (2021) 199,arXiv:2002.06197 [astro-ph.CO]

2021 arXiv
[89]

Impact of Cluster Physics on the Sunyaev-Zel’dovich Power Spectrum

L. Shaw, D. Nagai, S. Bhattacharya, and E. Lau, “Impact of Cluster Physics on the Sunyaev-Zel’dovich Power Spectrum”,Astrophys. J.725(2010) 1452,arXiv:1006.1945 [astro-ph.CO]

2010 arXiv
[90]

Angular Power Spectra of the Millimeter-Wavelength Background Light from Dusty Star-Forming Galaxies with the South Pole Telescope

N. Hall et al., “Angular Power Spectra of the Millimeter-Wavelength Background Light from Dusty Star-Forming Galaxies with the South Pole Telescope”,Astrophys. J.718(2010) 632, arXiv:0912.4315 [astro-ph.CO]

2010 arXiv
[91]

SPT-3G D1: A Measurement of Secondary Cosmic Microwave Background Anisotropy Power

P. Chaubal et al. (SPT-3G Collaboration), “SPT-3G D1: A Measurement of Secondary Cosmic Microwave Background Anisotropy Power”,arXiv:2601.20551 [astro-ph.CO]. 56

arXiv
[92]

The Atacama Cosmology Telescope: Likelihood for Small-Scale CMB Data

J. Dunkley et al., “The Atacama Cosmology Telescope: Likelihood for Small-Scale CMB Data”, JCAP07(2013) 025,arXiv:1301.0776 [astro-ph.CO]

2013 arXiv
[93]

The Atacama Cosmology Telescope: A Measurement of the Cosmic Microwave Background Power Spectra at 98 and 150 GHz

S. Choi et al. (ACT Collaboration), “The Atacama Cosmology Telescope: A Measurement of the Cosmic Microwave Background Power Spectra at 98 and 150 GHz”,JCAP12(2020) 045, arXiv:2007.07289 [astro-ph.CO]

2020 arXiv
[94]

Assessing the Importance of Noise from Thermal Sunyaev-Zel’dovich Signals for CMB Cluster Surveys and Cluster Cosmology

S. Raghunathan, “Assessing the Importance of Noise from Thermal Sunyaev-Zel’dovich Signals for CMB Cluster Surveys and Cluster Cosmology”,Astrophys. J.928(2022) 16,arXiv:2112.07656 [astro-ph.CO]

2022 arXiv
[95]

Planck 2015 Results. XXIII. The Thermal Sunyaev-Zeldovich Effect-Cosmic Infrared Background Correlation

P. A. R. Ade et al. (Planck Collaboration), “Planck 2015 Results. XXIII. The Thermal Sunyaev-Zeldovich Effect-Cosmic Infrared Background Correlation”,Astron. Astrophys.594(2016) A23,arXiv:1509.06555 [astro-ph.CO]

2016 arXiv
[96]

Measurement of the Full Shape of the Thermal-Sunyaev-Zel’dovich Power Spectrum from the South Pole Telescope and Herschel-SPIRE Observations

S. Raghunathan et al. (SPTpol and SPT-3G Collaborations), “Measurement of the Full Shape of the Thermal-Sunyaev-Zel’dovich Power Spectrum from the South Pole Telescope and Herschel-SPIRE Observations”,Astrophys. J. Lett.1002(2026) L22,arXiv:2602.10107 [astro-ph.CO]

2026
[97]

The Atacama Cosmology Telescope: Two-Season ACTPol Extragalactic Point Sources and Their Polarization Properties

R. Datta et al., “The Atacama Cosmology Telescope: Two-Season ACTPol Extragalactic Point Sources and Their Polarization Properties”,Mon. Not. Roy. Astron. Soc.486(2019) 5239, arXiv:1811.01854 [astro-ph.CO]

2019 arXiv
[98]

Fractional Polarization of Extragalactic Sources in the 500 deg2 SPTpol Survey

N. Gupta et al. (SPT Collaboration), “Fractional Polarization of Extragalactic Sources in the 500 deg2 SPTpol Survey”,Mon. Not. Roy. Astron. Soc.490(2019) 5712,arXiv:1907.02156 [astro-ph.CO]

2019 arXiv
[99]

A Method for Subtracting Foregrounds from Multi-Frequency CMB Sky Maps

M. Tegmark and G. Efstathiou, “A Method for Subtracting Foregrounds from Multi-Frequency CMB Sky Maps”,Mon. Not. Roy. Astron. Soc.281(1996) 1297,arXiv:astro-ph/9507009

1996 arXiv
[100]

Component Separation with Flexible Models – Application to Multi-Channel Astrophysical Observations

J.-F. Cardoso, M. Le Jeune, J. Delabrouille, M. Betoule, and G. Patanchon, “Component Separation with Flexible Models – Application to Multi-Channel Astrophysical Observations”,IEEE J. Sel. Top. Signal Process.2(2008) 735

2008
[101]

Planck 2013 Results. XII. Diffuse Component Separation

P. A. R. Ade et al. (Planck Collaboration), “Planck 2013 Results. XII. Diffuse Component Separation”,Astron. Astrophys.571(2014) A12,arXiv:1303.5072 [astro-ph.CO]

2014 arXiv
[102]

A Cross-Internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev-Zel’dovich Effect and CMB Lensing

S. Raghunathan and Y. Omori, “A Cross-Internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev-Zel’dovich Effect and CMB Lensing”,Astrophys. J.954(2023) 83,arXiv:2304.09166 [astro-ph.CO]

2023 arXiv
[103]

CMB and SZ Effect Separation with Constrained Internal Linear Combinations

M. Remazeilles, J. Delabrouille, and J.-F. Cardoso, “CMB and SZ Effect Separation with Constrained Internal Linear Combinations”,Mon. Not. Roy. Astron. Soc.410(2011) 2481, arXiv:1006.5599 [astro-ph.CO]

2011 arXiv
[104]

CMB/kSZ and Compton-yMaps from 2500 deg 2 of SPT-SZ and Planck Survey Data

L. Bleem et al. (SPT-SZ Collaboration), “CMB/kSZ and Compton-yMaps from 2500 deg 2 of SPT-SZ and Planck Survey Data”,Astrophys. J. Suppl. Ser.258(2022) 36,arXiv:2102.05033 [astro-ph.CO]

2022 arXiv
[105]

The Benefits of CMB Delensing

S. Hotinli, J. Meyers, C. Trendafilova, D. Green, and A. van Engelen, “The Benefits of CMB Delensing”,JCAP04(2022) 020,arXiv:2111.15036 [astro-ph.CO]

2022 arXiv
[106]

CLASS delens: Delensing Module for the CLASS Code

S. Hotinli, J. Meyers, C. Trendafilova, D. Green, and A. van Engelen, “CLASS delens: Delensing Module for the CLASS Code”, https:/ /github.com/selimhotinli/class delens (2021)

2021
[107]

CMB Delensing beyond the B Modes

D. Green, J. Meyers, and A. van Engelen, “CMB Delensing beyond the B Modes”,JCAP12(2017) 005,arXiv:1609.08143 [astro-ph.CO]. 57

2017 arXiv
[108]

The Impact of Cross-Covariances between the CMB and Reconstructed Lensing Power

C. Trendafilova, “The Impact of Cross-Covariances between the CMB and Reconstructed Lensing Power”,JCAP10(2023) 071,arXiv:2308.11588 [astro-ph.CO]

2023 arXiv
[109]

Snowmass 2021 CMB-HD White Paper

S. Aiola et al. (CMB-HD Collaboration), “Snowmass 2021 CMB-HD White Paper”, arXiv:2203.05728 [astro-ph.CO]

2021 arXiv
[110]

Improving Constraints on Models Addressing the Hubble Tension with CMB Delensing

J. Ange and J. Meyers, “Improving Constraints on Models Addressing the Hubble Tension with CMB Delensing”,JCAP10(2023) 045,arXiv:2307.01662 [astro-ph.CO]

2023 arXiv
[111]

Improving Constraints on Inflation with CMB Delensing

C. Trendafilova, S. Hotinli, and J. Meyers, “Improving Constraints on Inflation with CMB Delensing”,JCAP06(2024) 017,arXiv:2312.02954 [astro-ph.CO]

2024 arXiv
[112]

The Cosmic Linear Anisotropy Solving System (CLASS) II: Approximation Schemes

D. Blas, J. Lesgourgues, and T. Tram, “The Cosmic Linear Anisotropy Solving System (CLASS) II: Approximation Schemes”,JCAP07(2011) 034,arXiv:1104.2933 [astro-ph.CO]

2011 arXiv
[113]

CMB Lensing Power Spectrum Biases from Galaxies and Clusters using High-Angular-Resolution Temperature Maps

A. van Engelen, S. Bhattacharya, N. Sehgal, G. Holder, O. Zahn, and D. Nagai, “CMB Lensing Power Spectrum Biases from Galaxies and Clusters using High-Angular-Resolution Temperature Maps”,Astrophys. J.786(2014) 13,arXiv:1310.7023 [astro-ph.CO]

2014 arXiv
[114]

Beyond Fisher Forecasting for Cosmology

J. Ryan, B. Stevenson, C. Trendafilova, and J. Meyers, “Beyond Fisher Forecasting for Cosmology”, Phys. Rev. D107(2023) 103506,arXiv:2211.06534 [astro-ph.CO]

2023 arXiv
[115]

FisherLens: Fisher Forecasting Code for CLASS delens

S. Hotinli, J. Meyers, C. Trendafilova, D. Green, and A. van Engelen, “FisherLens: Fisher Forecasting Code for CLASS delens”, https:/ /github.com/ctrendafilova/FisherLens (2021)

2021
[116]

Breaking the Spell of Gaussianity: Forecasting with Higher-Order Fisher Matrices

E. Sellentin, M. Quartin, and L. Amendola, “Breaking the Spell of Gaussianity: Forecasting with Higher-Order Fisher Matrices”,Mon. Not. Roy. Astron. Soc.441(2014) 1831,arXiv:1401.6892 [astro-ph.CO]

2014
[117]

Calibrating the Non-Linear Matter Power Spectrum: Requirements for Future Weak Lensing Surveys

D. Huterer and M. Takada, “Calibrating the Non-Linear Matter Power Spectrum: Requirements for Future Weak Lensing Surveys”,Astropart. Phys.23(2005) 369,arXiv:astro-ph/0412142

2005 arXiv
[118]

Magnification-Temperature Correlation: The Dark Side of ISW Measurements

M. Loverde, L. Hui, and E. Gaztanaga, “Magnification-Temperature Correlation: The Dark Side of ISW Measurements”,Phys. Rev. D75(2007) 043519,arXiv:astro-ph/0611539

2007 arXiv
[119]

Systematic Bias in Cosmic Shear: Beyond the Fisher Matrix

A. Amara and A. R´ efr´ egier, “Systematic Bias in Cosmic Shear: Beyond the Fisher Matrix”,Mon. Not. Roy. Astron. Soc.391(2008) 228,arXiv:0710.5171 [astro-ph]

2008 arXiv
[120]

DRAFT: CMB-S4 Dark Radiation Anisotropy Flowdown Team Tool

S. Raghunathan, J. Meyers, C. Trendafilova, and B. Wallisch, “DRAFT: CMB-S4 Dark Radiation Anisotropy Flowdown Team Tool”, https:/ /github.com/sriniraghunathan/DRAFT (2026)

2026
[121]

PICO: Probe of Inflation and Cosmic Origins

S. Hanany et al. (PICO Collaboration), “PICO: Probe of Inflation and Cosmic Origins”, arXiv:1902.10541 [astro-ph.IM]

1902 arXiv
[122]

Cosmic Microwave Background Acoustic Peak Locations

Z. Pan, L. Knox, B. Mulroe, and A. Narimani, “Cosmic Microwave Background Acoustic Peak Locations”,Mon. Not. Roy. Astron. Soc.459(2016) 2513,arXiv:1603.03091 [astro-ph.CO]

2016 arXiv
[123]

Scaling Transformations and the Origins of Light Relics Constraints from Cosmic Microwave Background Observations

F. Ge, F.-Y. Cyr-Racine, and L. Knox, “Scaling Transformations and the Origins of Light Relics Constraints from Cosmic Microwave Background Observations”,Phys. Rev. D107(2023) 023517, arXiv:2210.16335 [astro-ph.CO]

2023 arXiv
[124]

Determining Neutrino Mass from the CMB Alone

M. Kaplinghat, L. Knox, and Y.-S. Song, “Determining Neutrino Mass from the CMB Alone”,Phys. Rev. Lett.91(2003) 241301,arXiv:astro-ph/0303344

2003 arXiv
[125]

Neutrino Mass from Cosmology

J. Lesgourgues and S. Pastor, “Neutrino Mass from Cosmology”,Adv. High Energy Phys.2012 (2012) 608515,arXiv:1212.6154 [hep-ph]

2012 arXiv
[126]

DESI and Other Dark Energy Experiments in the Era of Neutrino Mass Neasurements

A. Font-Ribera, P. McDonald, N. Mostek, B. Reid, H.-J. Seo, and A. Slosar, “DESI and Other Dark Energy Experiments in the Era of Neutrino Mass Neasurements”,JCAP05(2014) 023, 58 arXiv:1308.4164 [astro-ph.CO]

2014 arXiv
[127]

Cosmological Implications of a Neutrino Mass Detection

D. Green and J. Meyers, “Cosmological Implications of a Neutrino Mass Detection”, arXiv:2111.01096 [astro-ph.CO]

arXiv
[128]

CMB Polarization Can Constrain Cosmology Better than CMB Temperature

S. Galli, K. Benabed, F. Bouchet, J.-F. Cardoso, F. Elsner, E. Hivon, A. Mangilli, S. Prunet, and B. Wandelt, “CMB Polarization Can Constrain Cosmology Better than CMB Temperature”,Phys. Rev. D90(2014) 063504,arXiv:1403.5271 [astro-ph.CO]

2014 arXiv
[129]

The Information Content of Cosmic Microwave Background Anisotropies

D. Scott, D. Contreras, A. Narimani, and Y.-Z. Ma, “The Information Content of Cosmic Microwave Background Anisotropies”,JCAP06(2016) 046,arXiv:1603.03550 [astro-ph.CO]

2016 arXiv
[130]

The LBTYp Project IV: A New Value of the Primordial Helium Abundance

E. Aver, E. Skillman, R. Pogge, N. Rogers, M. Weller, K. Olive, D. Berg, J. Salzer, J. Miller, and J. M´ endez-Delgado, “The LBTYp Project IV: A New Value of the Primordial Helium Abundance”, arXiv:2601.22238 [astro-ph.CO]
[131]

Spectral Distortions of the CMB as a Probe of Inflation, Recombination, Structure Formation, and Particle Physics: Astro2020 Science White Paper

J. Chluba et al., “Spectral Distortions of the CMB as a Probe of Inflation, Recombination, Structure Formation, and Particle Physics: Astro2020 Science White Paper”,Bull. Am. Astron. Soc. 51(2019) 184,arXiv:1903.04218 [astro-ph.CO]

2019 arXiv
[132]

New Horizons in Cosmology with Spectral Distortions of the Cosmic Microwave Background

J. Chluba et al., “New Horizons in Cosmology with Spectral Distortions of the Cosmic Microwave Background”,Exper. Astron.51(2021) 1515,arXiv:1909.01593 [astro-ph.CO]

2021 arXiv
[133]

The Cosmic Microwave Background: Spectral Distortions

J. Chluba, “The Cosmic Microwave Background: Spectral Distortions”,Encyclopedia of Astrophysics5(2026) 184,arXiv:2502.05188 [astro-ph.CO]

2026 arXiv
[134]

Finding eV-Scale Light Relics with Cosmological Observables

N. DePorzio, W. L. Xu, J. Mu˜ noz, and C. Dvorkin, “Finding eV-Scale Light Relics with Cosmological Observables”,Phys. Rev. D103(2021) 023504,arXiv:2006.09380 [astro-ph.CO]

2021 arXiv
[135]

Cosmological Constraints on Light but Massive Relics

W. L. Xu, J. Mu˜ noz, and C. Dvorkin, “Cosmological Constraints on Light but Massive Relics”, Phys. Rev. D105(2022) 095029,arXiv:2107.09664 [astro-ph.CO]

2022 arXiv
[136]

Forecasting Constraints on Non-Thermal Light Massive Relics from Future CMB Experiments (CMB-S4/Simons Observatory)

A. Banerjee, A. Bhattacharjee, S. Das, A. Maharana, and R. K. Sharma, “Forecasting Constraints on Non-Thermal Light Massive Relics from Future CMB Experiments (CMB-S4/Simons Observatory)”,Phys. Rev. D113(2026) 043506,arXiv:2505.22775 [astro-ph.CO]

2026
[137]

Clustering with Light (but Massive) Relics

J. Kumar, P. Sandick, and S. Xu, “Clustering with Light (but Massive) Relics”, arXiv:2512.14672 [astro-ph.CO]
[138]

Using SquiRels to Find LiMRs: A Model-Insensitive Approach to Cosmic Microwave Background Studies of Light but Massive Relics

N. DePorzio, D. Imig, and J. Shelton, “Using SquiRels to Find LiMRs: A Model-Insensitive Approach to Cosmic Microwave Background Studies of Light but Massive Relics”, arXiv:2607.12021 [astro-ph.CO]

arXiv
[139]

The Low-Energy Frontier of Particle Physics

J. Jaeckel and A. Ringwald, “The Low-Energy Frontier of Particle Physics”,Ann. Rev. Nucl. Part. Sci.60(2010) 405,arXiv:1002.0329 [hep-ph]

2010 arXiv
[140]

New Light Species and the CMB

C. Brust, D. Kaplan, and M. Walters, “New Light Species and the CMB”,JHEP12(2013) 058, arXiv:1303.5379 [hep-ph]

2013 arXiv
[141]

Working Group Report: New Light Weakly Coupled Particles

R. Essig et al., “Working Group Report: New Light Weakly Coupled Particles”, arXiv:1311.0029 [hep-ph]

arXiv
[142]

CP Conservation in the Presence of Instantons

R. Peccei and H. Quinn, “CP Conservation in the Presence of Instantons”,Phys. Rev. Lett.38 (1977) 1440

1977
[143]

A New Light Boson?

S. Weinberg, “A New Light Boson?”,Phys. Rev. Lett.40(1978) 223

1978
[144]

Problem of Strong P and T Invariance in the Presence of Instantons

F. Wilczek, “Problem of Strong P and T Invariance in the Presence of Instantons”,Phys. Rev. Lett. 40(1978) 279. 59

1978
[145]

TASI Lectures on the Strong CP Problem and Axions

A. Hook, “TASI Lectures on the Strong CP Problem and Axions”,PoSTASI2018(2019) 004, arXiv:1812.02669 [hep-ph]

2019 arXiv
[146]

Cosmological Relaxation of the Electroweak Scale

P. Graham, D. Kaplan, and S. Rajendran, “Cosmological Relaxation of the Electroweak Scale”, Phys. Rev. Lett.115(2015) 221801,arXiv:1504.07551 [hep-ph]

2015 arXiv
[147]

Solving the Hierarchy Problem at Reheating with a Large Number of Degrees of Freedom

N. Arkani-Hamed, T. Cohen, R. D’Agnolo, A. Hook, H. D. Kim, and D. Pinner, “Solving the Hierarchy Problem at Reheating with a Large Number of Degrees of Freedom”,Phys. Rev. Lett.117 (2016) 251801,arXiv:1607.06821 [hep-ph]

2016 arXiv
[148]

Cosmology in Mirror Twin Higgs and Neutrino Masses

Z. Chacko, N. Craig, P. Fox, and R. Harnik, “Cosmology in Mirror Twin Higgs and Neutrino Masses”,JHEP07(2017) 023,arXiv:1611.07975 [hep-ph]

2017 arXiv
[149]

The Landscape of QCD Axion Models

L. Di Luzio, M. Giannotti, E. Nardi, and L. Visinelli, “The Landscape of QCD Axion Models”, Phys. Rept.870(2020) 1,arXiv:2003.01100 [hep-ph]

2020 arXiv
[150]

Axion Dark Matter

C. Adams et al., “Axion Dark Matter”,arXiv:2203.14923 [hep-ex]

arXiv
[151]

Minimal Flavor Unification via Multi-Generational Peccei-Quinn Symmetry

A. Davidson and K. Wali, “Minimal Flavor Unification via Multi-Generational Peccei-Quinn Symmetry”,Phys. Rev. Lett.48(1982) 11

1982
[152]

Axions and Family Symmetry Breaking

F. Wilczek, “Axions and Family Symmetry Breaking”,Phys. Rev. Lett.49(1982) 1549

1982
[153]

Can the Family Group Be a Global Symmetry?

D. Reiss, “Can the Family Group Be a Global Symmetry?”,Phys. Lett. B115(1982) 217

1982
[154]

Third-Generation Familons, B Factories, and Neutrino Cosmology

J. Feng, T. Moroi, H. Murayama, and E. Schnapka, “Third-Generation Familons, B Factories, and Neutrino Cosmology”,Phys. Rev. D57(1998) 5875,arXiv:hep-ph/9709411

1998 arXiv
[155]

Are There Real Goldstone Bosons Associated with Broken Lepton Number?

Y. Chikashige, R. Mohapatra, and R. Peccei, “Are There Real Goldstone Bosons Associated with Broken Lepton Number?”,Phys. Lett. B98(1981) 265

1981
[156]

CMB Signals of Neutrino Mass Generation

Z. Chacko, L. Hall, T. Okui, and S. Oliver, “CMB Signals of Neutrino Mass Generation”,Phys. Rev. D70(2004) 085008,arXiv:hep-ph/0312267

2004 arXiv
[157]

Axions in String Theory

P. Svrcek and E. Witten, “Axions in String Theory”,JHEP06(2006) 051, arXiv:hep-th/0605206

2006 arXiv
[158]

String Axiverse

A. Arvanitaki, S. Dimopoulos, S. Dubovsky, N. Kaloper, and J. March-Russell, “String Axiverse”, Phys. Rev. D81(2010) 123530,arXiv:0905.4720 [hep-th]

2010 arXiv
[159]

Dark Radiation in LARGE-Volume Models

M. Cicoli, J. Conlon, and F. Quevedo, “Dark Radiation in LARGE-Volume Models”,Phys. Rev. D 87(2013) 043520,arXiv:1208.3562 [hep-ph]

2013 arXiv
[160]

Compactified String Theories – Generic Predictions for Particle Physics

B. S. Acharya, G. Kane, and P. Kumar, “Compactified String Theories – Generic Predictions for Particle Physics”,Int. J. Mod. Phys. A27(2012) 1230012,arXiv:1204.2795 [hep-ph]

2012 arXiv
[161]

Axion Cosmology

D. J. E. Marsh, “Axion Cosmology”,Phys. Rept.643(2016) 1,arXiv:1510.07633 [astro-ph.CO]

2016 arXiv
[162]

Cosmology of the Invisible Axion

J. Preskill, M. Wise, and F. Wilczek, “Cosmology of the Invisible Axion”,Phys. Lett. B120(1983) 127

1983
[163]

A Cosmological Bound on the Invisible Axion

L. Abbott and P. Sikivie, “A Cosmological Bound on the Invisible Axion”,Phys. Lett. B120(1983) 133

1983
[164]

The Not-So-Harmless Axion

M. Dine and W. Fischler, “The Not-So-Harmless Axion”,Phys. Lett. B120(1983) 137

1983
[165]

Cosmological Bounds on Pseudo-Nambu-Goldstone Bosons

D. Cadamuro and J. Redondo, “Cosmological Bounds on Pseudo-Nambu-Goldstone Bosons”,JCAP 02(2012) 032,arXiv:1110.2895 [hep-ph]

2012 arXiv
[166]

Hidden Dark-Matter Sector, Dark Radiation, and the CMB

Z. Chacko, Y. Cui, S. Hong, and T. Okui, “Hidden Dark-Matter Sector, Dark Radiation, and the CMB”,Phys. Rev. D92(2015) 055033,arXiv:1505.04192 [hep-ph]. 60

2015 arXiv
[167]

New Target for Cosmic Axion Searches

D. Baumann, D. Green, and B. Wallisch, “New Target for Cosmic Axion Searches”,Phys. Rev. Lett. 117(2016) 171301,arXiv:1604.08614 [astro-ph.CO]

2016 arXiv
[168]

Observable Windows for the QCD Axion through the Number of Relativistic Species

R. Ferreira and A. Notari, “Observable Windows for the QCD Axion through the Number of Relativistic Species”,Phys. Rev. Lett.120(2018) 191301,arXiv:1801.06090 [hep-ph]

2018 arXiv
[169]

Hot Axions and theH 0 Tension

F. D’Eramo, R. Ferreira, A. Notari, and J. Bernal, “Hot Axions and theH 0 Tension”,JCAP11 (2018) 014,arXiv:1808.07430 [hep-ph]

2018 arXiv
[170]

Production of Thermal Axions across the Electroweak Phase Transition

F. Arias-Arag´ on, F. D’Eramo, R. Ferreira, L. Merlo, and A. Notari, “Production of Thermal Axions across the Electroweak Phase Transition”,JCAP03(2021) 090,arXiv:2012.04736 [hep-ph]

2021 arXiv
[171]

Dine-Fischler-Srednicki-Zhitnitsky Axion in the CMB

R. Ferreira, A. Notari, and F. Rompineve, “Dine-Fischler-Srednicki-Zhitnitsky Axion in the CMB”, Phys. Rev. D103(2021) 063524,arXiv:2012.06566 [hep-ph]

2021 arXiv
[172]

Cosmic Axion Background

J. Dror, H. Murayama, and N. Rodd, “Cosmic Axion Background”,Phys. Rev. D103(2021) 115004,arXiv:2101.09287 [hep-ph]

2021 arXiv
[173]

Novel Cosmological Bounds on Thermally-Produced Axion-Like Particles

L. Caloni, M. Gerbino, M. Lattanzi, and L. Visinelli, “Novel Cosmological Bounds on Thermally-Produced Axion-Like Particles”,JCAP09(2022) 021,arXiv:2205.01637 [astro-ph.CO]

2022 arXiv
[174]

Constraints on Axion-Lepton Coupling from Big Bang Nucleosynthesis

D. Ghosh and D. Sachdeva, “Constraints on Axion-Lepton Coupling from Big Bang Nucleosynthesis”,JCAP10(2020) 060,arXiv:2007.01873 [hep-ph]

2020 arXiv
[175]

Cosmological Implications of Axion-Matter Couplings

D. Green, Y. Guo, and B. Wallisch, “Cosmological Implications of Axion-Matter Couplings”,JCAP 02(2022) 019,arXiv:2109.12088 [astro-ph.CO]

2022 arXiv
[176]

Flavor-Violating Axions in the Early Universe

F. D’Eramo and S. Yun, “Flavor-Violating Axions in the Early Universe”,Phys. Rev. D105(2022) 075002,arXiv:2111.12108 [hep-ph]

2022 arXiv
[177]

Precise Predictions for the QCD Axion Contribution to Dark Radiation with Full Phase-Space Evolution

M. Badziak and M. Laletin, “Precise Predictions for the QCD Axion Contribution to Dark Radiation with Full Phase-Space Evolution”,JHEP02(2025) 108,arXiv:2410.18186 [hep-ph]

2025 arXiv
[178]

Back to the Phase Space: Thermal-Axion Dark Radiation via Couplings to Standard Model Fermions

F. D’Eramo and A. Lenoci, “Back to the Phase Space: Thermal-Axion Dark Radiation via Couplings to Standard Model Fermions”,Phys. Rev. D110(2024) 116028,arXiv:2410.21253 [hep-ph]

2024
[179]

Improved Cosmological Constraints on Axion-Lepton Interactions

M. Badziak, A. Gomu lka, M. Laletin, and K. Szafra´ nski, “Improved Cosmological Constraints on Axion-Lepton Interactions”,Phys. Dark Univ.52(2026) 102335,arXiv:2511.14864 [hep-ph]

2026 arXiv
[180]

Beyond Thermal Approximations: Precise Cosmological Bounds on Axion-Like Particles

N. Barbieri, L. Caloni, M. Gerbino, M. Lattanzi, and L. Visinelli, “Beyond Thermal Approximations: Precise Cosmological Bounds on Axion-Like Particles”,JCAP07(2026) 099, arXiv:2602.11100 [astro-ph.CO]

2026 arXiv
[181]

Light Sterile Neutrinos: A White Paper

K. Abazajian et al., “Light Sterile Neutrinos: A White Paper”,arXiv:1204.5379 [hep-ph]

arXiv
[182]

Dipole Portal to Heavy Neutral Leptons

G. Magill, R. Plestid, M. Pospelov, and Y.-D. Tsai, “Dipole Portal to Heavy Neutral Leptons”, Phys. Rev. D98(2018) 115015,arXiv:1803.03262 [hep-ph]

2018 arXiv
[183]

Dirac Neutrinos andN eff

X. Luo, W. Rodejohann, and X.-J. Xu, “Dirac Neutrinos andN eff”,JCAP06(2020) 058, arXiv:2005.01629 [hep-ph]

2020 arXiv
[184]

The Neutrino Magnetic Moment Portal: Cosmology, Astrophysics and Direct Detection

V. Brdar, A. Greljo, J. Kopp, and T. Opferkuch, “The Neutrino Magnetic Moment Portal: Cosmology, Astrophysics and Direct Detection”,JCAP01(2021) 039,arXiv:2007.15563 [hep-ph]

2021 arXiv
[185]

Sterile Neutrinos in Cosmology

K. Abazajian, “Sterile Neutrinos in Cosmology”,Phys. Rept.711(2017) 1,arXiv:1705.01837 [hep-ph]

2017 arXiv
[186]

Thermalization of Sterile Neutrinos in the Early Universe 61 in the 3+1 Scheme with Full Mixing Matrix

S. Gariazzo, P. de Salas, and S. Pastor, “Thermalization of Sterile Neutrinos in the Early Universe 61 in the 3+1 Scheme with Full Mixing Matrix”,JCAP07(2019) 014,arXiv:1905.11290 [astro-ph.CO]

2019 arXiv
[187]

Bounds on Light Sterile Neutrino Mass and Mixing from Cosmology and Laboratory Searches

S. Hagstotz, P. de Salas, S. Gariazzo, M. Gerbino, M. Lattanzi, S. Vagnozzi, K. Freese, and S. Pastor, “Bounds on Light Sterile Neutrino Mass and Mixing from Cosmology and Laboratory Searches”,Phys. Rev. D104(2021) 123524,arXiv:2003.02289 [astro-ph.CO]

2021 arXiv
[188]

Dark Radiation from Neutrino Mixing after Big Bang Nucleosynthesis

D. Aloni, M. Joseph, M. Schmaltz, and N. Weiner, “Dark Radiation from Neutrino Mixing after Big Bang Nucleosynthesis”,Phys. Rev. Lett.131(2023) 221001,arXiv:2301.10792 [astro-ph.CO]

2023 arXiv
[189]

Extra Radiation Cosmologies: Implications of the Hubble Tension for eV-Scale Neutrinos

H. Garc´ ıa Escudero and K. Abazajian, “Extra Radiation Cosmologies: Implications of the Hubble Tension for eV-Scale Neutrinos”,Phys. Rev. D113(2026) 023508,arXiv:2509.25478 [hep-ph]

2026
[190]

Observing Dirac Neutrinos in the Cosmic Microwave Background

K. Abazajian and J. Heeck, “Observing Dirac Neutrinos in the Cosmic Microwave Background”, Phys. Rev. D100(2019) 075027,arXiv:1908.03286 [hep-ph]

2019 arXiv
[191]

Unraveling the Dirac Neutrino with Cosmological and Terrestrial Detectors

P. Adshead, Y. Cui, A. Long, and M. Shamma, “Unraveling the Dirac Neutrino with Cosmological and Terrestrial Detectors”,Phys. Lett. B823(2021) 136736,arXiv:2009.07852 [hep-ph]

2021 arXiv
[192]

Light Dirac Neutrino Portal Dark Matter with Observable ∆Neff

A. Biswas, D. Borah, and D. Nanda, “Light Dirac Neutrino Portal Dark Matter with Observable ∆Neff”,JCAP10(2021) 002,arXiv:2103.05648 [hep-ph]

2021 arXiv
[193]

TwoU(1)s andϵCharge Shifts

B. Holdom, “TwoU(1)s andϵCharge Shifts”,Phys. Lett. B166(1986) 196

1986
[194]

TwoZs or Not TwoZs?

P. Galison and A. Manohar, “TwoZs or Not TwoZs?”,Phys. Lett. B136(1984) 279

1984
[195]

Dark Matter and Dark Radiation

L. Ackerman, M. Buckley, S. Carroll, and M. Kamionkowski, “Dark Matter and Dark Radiation”, Phys. Rev. D79(2009) 023519,arXiv:0810.5126 [hep-ph]

2009 arXiv
[196]

SecludedU(1) below the Weak Scale

M. Pospelov, “SecludedU(1) below the Weak Scale”,Phys. Rev. D80(2009) 095002, arXiv:0811.1030 [hep-ph]

2009 arXiv
[197]

Dark-Radiation Constraints on Minicharged Particles in Models with a Hidden Photon

H. Vogel and J. Redondo, “Dark-Radiation Constraints on Minicharged Particles in Models with a Hidden Photon”,JCAP02(2014) 029,arXiv:1311.2600 [hep-ph]

2014 arXiv
[198]

Hidden Dipole Dark Matter

A. Pierce and Z. Zhang, “Hidden Dipole Dark Matter”,Phys. Rev. D90(2014) 015026, arXiv:1405.1937 [hep-ph]

2014 arXiv
[199]

Dark-Radiation Constraints on Portal Interactions with Hidden Sectors

P. Adshead, P. Ralegankar, and J. Shelton, “Dark-Radiation Constraints on Portal Interactions with Hidden Sectors”,JCAP09(2022) 056,arXiv:2206.13530 [hep-ph]

2022 arXiv
[200]

The Dark Photon: A 2026 Perspective

A. Caputo and R. Essig, “The Dark Photon: A 2026 Perspective”,arXiv:2603.08430 [hep-ph]

2026 arXiv
[201]

Massive Hidden Photons as Lukewarm Dark Matter

J. Redondo and M. Postma, “Massive Hidden Photons as Lukewarm Dark Matter”,JCAP02(2009) 005,arXiv:0811.0326 [hep-ph]

2009 arXiv
[202]

Cosmological Constraints on Decoupled Dark Photons and Dark Higgs

J. Berger, K. Jedamzik, and D. Walker, “Cosmological Constraints on Decoupled Dark Photons and Dark Higgs”,JCAP11(2016) 032,arXiv:1605.07195 [hep-ph]

2016 arXiv
[203]

Cosmological Constraint on Dark Photon fromN eff

M. Ibe, S. Kobayashi, Y. Nakayama, and S. Shirai, “Cosmological Constraint on Dark Photon fromN eff”,JHEP04(2020) 009,arXiv:1912.12152 [hep-ph]

2020 arXiv
[204]

Dark-Photon Limits: A Handbook

A. Caputo, A. Millar, C. O’Hare, and E. Vitagliano, “Dark-Photon Limits: A Handbook”,Phys. Rev. D104(2021) 095029,arXiv:2105.04565 [hep-ph]

2021 arXiv
[205]

Cosmological Constraints on the Scale of Supersymmetry Breaking

S. Weinberg, “Cosmological Constraints on the Scale of Supersymmetry Breaking”,Phys. Rev. Lett. 48(1982) 1303

1982
[206]

Cosmological Constraints on the Light Stable Gravitino

T. Moroi, H. Murayama, and M. Yamaguchi, “Cosmological Constraints on the Light Stable Gravitino”,Phys. Lett. B303(1993) 289. 62

1993
[207]

Thermal Production of Gravitinos

M. Bolz, A. Brandenburg, and W. Buchmuller, “Thermal Production of Gravitinos”,Nucl. Phys. B 606(2001) 518,arXiv:hep-ph/0012052

2001 arXiv
[208]

Light Gravitinos at Colliders and Implications for Cosmology

J. Feng, M. Kamionkowski, and S. Lee, “Light Gravitinos at Colliders and Implications for Cosmology”,Phys. Rev. D82(2010) 015012,arXiv:1004.4213 [hep-ph]

2010 arXiv
[209]

The Formation of Cosmic Structures in a Light-Gravitino-Dominated Universe

E. Pierpaoli, S. Borgani, A. Masiero, and M. Yamaguchi, “The Formation of Cosmic Structures in a Light-Gravitino-Dominated Universe”,Phys. Rev. D57(1998) 2089,arXiv:astro-ph/9709047

1998 arXiv
[210]

Constraining Light Gravitino Mass from Cosmic Microwave Background

K. Ichikawa, M. Kawasaki, K. Nakayama, T. Sekiguchi, and T. Takahashi, “Constraining Light Gravitino Mass from Cosmic Microwave Background”,JCAP08(2009) 013,arXiv:0905.2237 [astro-ph.CO]

2009 arXiv
[211]

Cosmological Constraint on the Light Gravitino Mass from CMB Lensing and Cosmic Shear

K. Osato, T. Sekiguchi, M. Shirasaki, A. Kamada, and N. Yoshida, “Cosmological Constraint on the Light Gravitino Mass from CMB Lensing and Cosmic Shear”,JCAP06(2016) 004, arXiv:1601.07386 [astro-ph.CO]

2016 arXiv
[212]

Constraining the Phase Shift of Relativistic Species in DESI BAOs

A. Whitford et al., “Constraining the Phase Shift of Relativistic Species in DESI BAOs”,Mon. Not. Roy. Astron. Soc.538(2025) 1980,arXiv:2412.05990 [astro-ph.CO]

2025 arXiv
[213]

Tracing the Neutrino-Induced Phase Shift in the 21 cm Spectrum

G. Montefalcone, H. A. Cruz, J. Mu˜ noz, E. Kovetz, and M. Kamionkowski, “Tracing the Neutrino-Induced Phase Shift in the 21 cm Spectrum”,Phys. Rev. D113(2026) 063556, arXiv:2509.03595 [astro-ph.CO]

2026 arXiv
[214]

Cosmological Signatures of Interacting Neutrinos

N. Bell, E. Pierpaoli, and K. Sigurdson, “Cosmological Signatures of Interacting Neutrinos”,Phys. Rev. D73(2006) 063523,arXiv:astro-ph/0511410

2006 arXiv
[215]

Constraining Models of Neutrino Mass and Neutrino Interactions with the Planck Satellite

A. Friedland, K. Zurek, and S. Bashinsky, “Constraining Models of Neutrino Mass and Neutrino Interactions with the Planck Satellite”,arXiv:0704.3271 [astro-ph]

arXiv
[216]

Cosmological Constraints on Interacting Light Particles

C. Brust, Y. Cui, and K. Sigurdson, “Cosmological Constraints on Interacting Light Particles”, JCAP08(2017) 020,arXiv:1703.10732 [astro-ph.CO]

2017 arXiv
[217]

Interacting Radiation after Planck and Its Implications for the Hubble Tension

N. Blinov and G. Marques-Tavares, “Interacting Radiation after Planck and Its Implications for the Hubble Tension”,JCAP09(2020) 029,arXiv:2003.08387 [astro-ph.CO]

2020 arXiv
[218]

Self-Interacting Neutrinos, the Hubble Parameter Tension, and the Cosmic Microwave Background

T. Brinckmann, J. H. Chang, and M. Loverde, “Self-Interacting Neutrinos, the Hubble Parameter Tension, and the Cosmic Microwave Background”,Phys. Rev. D104(2021) 063523, arXiv:2012.11830 [astro-ph.CO]

2021 arXiv
[219]

Abundance and Properties of Dark Radiation from the Cosmic Microwave Background

M. Saravanan, T. Brinckmann, M. Loverde, and Z. Weiner, “Abundance and Properties of Dark Radiation from the Cosmic Microwave Background”,JCAP08(2025) 040,arXiv:2503.04671 [astro-ph.CO]

2025 arXiv
[220]

Exploring the Dark Sector: Interacting Radiation in Light of Modern Cosmological Probes

M. Mescia and H. Gil-Mar´ ın, “Exploring the Dark Sector: Interacting Radiation in Light of Modern Cosmological Probes”,arXiv:2605.24089 [astro-ph.CO]

arXiv
[221]

Self-Interacting Dark Radiation

K. S. Jeong and F. Takahashi, “Self-Interacting Dark Radiation”,Phys. Lett. B725(2013) 134, arXiv:1305.6521 [hep-ph]

2013 arXiv
[222]

Non-Abelian Dark Matter and Dark Radiation

M. Buen-Abad, G. Marques-Tavares, and M. Schmaltz, “Non-Abelian Dark Matter and Dark Radiation”,Phys. Rev. D92(2015) 023531,arXiv:1505.03542 [hep-ph]

2015 arXiv
[223]

Evidence for Dark-Matter Interactions in Cosmological Precision Data?

J. Lesgourgues, G. Marques-Tavares, and M. Schmaltz, “Evidence for Dark-Matter Interactions in Cosmological Precision Data?”,JCAP02(2016) 037,arXiv:1507.04351 [astro-ph.CO]

2016 arXiv
[224]

Limits on Neutrino-Neutrino Scattering in the Early Universe

F.-Y. Cyr-Racine and K. Sigurdson, “Limits on Neutrino-Neutrino Scattering in the Early Universe”,Phys. Rev. D90(2014) 123533,arXiv:1306.1536 [astro-ph.CO]. 63

2014 arXiv
[225]

A Tale of Two Modes: Neutrino Free-Streaming in the Early Universe

L. Lancaster, F.-Y. Cyr-Racine, L. Knox, and Z. Pan, “A Tale of Two Modes: Neutrino Free-Streaming in the Early Universe”,JCAP07(2017) 033,arXiv:1704.06657 [astro-ph.CO]

2017 arXiv
[226]

Probing Decoupling in Dark Sectors with the Cosmic Microwave Background

G. Choi, C.-T. Chiang, and M. Loverde, “Probing Decoupling in Dark Sectors with the Cosmic Microwave Background”,JCAP06(2018) 044,arXiv:1804.10180 [astro-ph.CO]

2018 arXiv
[227]

Neutrino Puzzle: Anomalies, Interactions, and Cosmological Tensions

C. Kreisch, F.-Y. Cyr-Racine, and O. Dor´ e, “Neutrino Puzzle: Anomalies, Interactions, and Cosmological Tensions”,Phys. Rev. D101(2020) 123505,arXiv:1902.00534 [astro-ph.CO]

2020 arXiv
[228]

Can Dark Neutrino Interactions Phase Out the Hubble Tension?

S. Ghosh, R. Khatri, and T. Roy, “Can Dark Neutrino Interactions Phase Out the Hubble Tension?”,Phys. Rev. D102(2020) 123544,arXiv:1908.09843 [hep-ph]

2020 arXiv
[229]

Global View of Neutrino Interactions in Cosmology: The Free-Streaming Window as Seen by Planck

P. Taule, M. Escudero, and M. Garny, “Global View of Neutrino Interactions in Cosmology: The Free-Streaming Window as Seen by Planck”,Phys. Rev. D106(2022) 063539, arXiv:2207.04062 [astro-ph.CO]

2022 arXiv
[230]

Confronting Interacting Dark-Radiation Scenarios with Cosmological Data

T. Brinckmann, J. H. Chang, P. Du, and M. Loverde, “Confronting Interacting Dark-Radiation Scenarios with Cosmological Data”,Phys. Rev. D107(2023) 123517,arXiv:2212.13264 [astro-ph.CO]

2023 arXiv
[231]

Interacting Dark Sector and Precision Cosmology

M. Buen-Abad, M. Schmaltz, J. Lesgourgues, and T. Brinckmann, “Interacting Dark Sector and Precision Cosmology”,JCAP01(2018) 008,arXiv:1708.09406 [astro-ph.CO]

2018 arXiv
[232]

A Step in Understanding the Hubble Tension

D. Aloni, A. Berlin, M. Joseph, M. Schmaltz, and N. Weiner, “A Step in Understanding the Hubble Tension”,Phys. Rev. D105(2022) 123516,arXiv:2111.00014 [astro-ph.CO]

2022 arXiv
[233]

InterACTing Dark-Radiation Models after ACT

W. Cvetko, M. Joseph, and G. Marques-Tavares, “InterACTing Dark-Radiation Models after ACT”, arXiv:2512.19633 [astro-ph.CO]
[234]

Recoupled Dark Radiation Reconciling CMB and DESI BAO Measurements

R. Sharma, M. Archidiacono, and J. Lesgourgues, “Recoupled Dark Radiation Reconciling CMB and DESI BAO Measurements”,arXiv:2605.18716 [astro-ph.CO]

arXiv
[235]

Updated Constraints on Non-Standard Neutrino Interactions from Planck

M. Archidiacono and S. Hannestad, “Updated Constraints on Non-Standard Neutrino Interactions from Planck”,JCAP07(2014) 046,arXiv:1311.3873 [astro-ph.CO]

2014 arXiv
[236]

Interacting Neutrinos in Cosmology: Exact Description and Constraints

I. Oldengott, T. Tram, C. Rampf, and Y. Y. Y. Wong, “Interacting Neutrinos in Cosmology: Exact Description and Constraints”,JCAP11(2017) 027,arXiv:1706.02123 [astro-ph.CO]

2017 arXiv
[237]

Constraints on Secret Neutrino Interactions after Planck

F. Forastieri, M. Lattanzi, and P. Natoli, “Constraints on Secret Neutrino Interactions after Planck”, JCAP07(2015) 014,arXiv:1504.04999 [astro-ph.CO]

2015 arXiv
[238]

Cosmological Constraints on Neutrino Self-Interactions with a Light Mediator

F. Forastieri, M. Lattanzi, and P. Natoli, “Cosmological Constraints on Neutrino Self-Interactions with a Light Mediator”,Phys. Rev. D100(2019) 103526,arXiv:1904.07810 [astro-ph.CO]

2019 arXiv
[239]

Flavor-Specific Interaction Favors Strong Neutrino Self-Coupling in the Early Universe

A. Das and S. Ghosh, “Flavor-Specific Interaction Favors Strong Neutrino Self-Coupling in the Early Universe”,JCAP07(2021) 038,arXiv:2011.12315 [astro-ph.CO]

2021 arXiv
[240]

Updated Constraints on Massive Neutrino Self-Interactions from Cosmology in Light of theH 0 Tension

S. Roy Choudhury, S. Hannestad, and T. Tram, “Updated Constraints on Massive Neutrino Self-Interactions from Cosmology in Light of theH 0 Tension”,JCAP03(2021) 084, arXiv:2012.07519 [astro-ph.CO]

2021 arXiv
[241]

Massive Neutrino Self-Interactions with a Light Mediator in Cosmology

J. Venzor, G. Garcia-Arroyo, A. P´ erez-Lorenzana, and J. De-Santiago, “Massive Neutrino Self-Interactions with a Light Mediator in Cosmology”,Phys. Rev. D105(2022) 123539, arXiv:2202.09310 [astro-ph.CO]

2022 arXiv
[242]

The Magnificent ACT of Flavor-Specific Neutrino Self-Interaction

A. Das and S. Ghosh, “The Magnificent ACT of Flavor-Specific Neutrino Self-Interaction”,JCAP 09(2023) 042,arXiv:2303.08843 [astro-ph.CO]

2023 arXiv
[243]

Self-Interacting Neutrinos in Light of 64 Large-Scale-Structure Data

A. He, R. An, M. Ivanov, and V. Gluscevic, “Self-Interacting Neutrinos in Light of 64 Large-Scale-Structure Data”,Phys. Rev. D109(2024) 103527, arXiv:2309.03956 [astro-ph.CO]

2024 arXiv
[244]

Confronting Self-Interacting Neutrinos with the Full Shape of the Galaxy Power Spectrum

D. Camarena, F.-Y. Cyr-Racine, and J. Houghteling, “Confronting Self-Interacting Neutrinos with the Full Shape of the Galaxy Power Spectrum”,Phys. Rev. D108(2023) 103535, arXiv:2309.03941 [astro-ph.CO]

2023 arXiv
[245]

Strong Constraints on a Simple Self-Interacting Neutrino Cosmology

D. Camarena and F.-Y. Cyr-Racine, “Strong Constraints on a Simple Self-Interacting Neutrino Cosmology”,Phys. Rev. D111(2025) 023504,arXiv:2403.05496 [astro-ph.CO]

2025 arXiv
[246]

Self-Interacting Neutrinos in Light of Recent CMB and LSS Data

A. Poudou, T. Simon, T. Montandon, E. Teixeira, and V. Poulin, “Self-Interacting Neutrinos in Light of Recent CMB and LSS Data”,Phys. Rev. D112(2025) 103535,arXiv:2503.10485 [astro-ph.CO]

2025 arXiv
[247]

Limits on Self-Interacting Neutrinos from the BAO and CMB Phase Shift

A. Whitford, C. Howlett, T. Davis, D. Camarena, and F.-Y. Cyr-Racine, “Limits on Self-Interacting Neutrinos from the BAO and CMB Phase Shift”,JCAP03(2026) 064,arXiv:2511.00800 [astro-ph.CO]

2026
[248]

Neutrino Self-Interactions: A White Paper

J. Berryman et al., “Neutrino Self-Interactions: A White Paper”,Phys. Dark Univ.42(2023) 101267,arXiv:2203.01955 [hep-ph]

2023 arXiv
[249]

Cosmological Bounds on Dark Matter-Neutrino Interactions

G. Mangano, A. Melchiorri, P. Serra, A. Cooray, and M. Kamionkowski, “Cosmological Bounds on Dark Matter-Neutrino Interactions”,Phys. Rev. D74(2006) 043517,arXiv:astro-ph/0606190

2006 arXiv
[250]

Cosmology of Atomic Dark Matter

F.-Y. Cyr-Racine and K. Sigurdson, “Cosmology of Atomic Dark Matter”,Phys. Rev. D87(2013) 103515,arXiv:1209.5752 [astro-ph.CO]

2013 arXiv
[251]

Constraining Dark Matter-Neutrino Interactions using the CMB and Large-Scale Structure

R. Wilkinson, C. Bœhm, and J. Lesgourgues, “Constraining Dark Matter-Neutrino Interactions using the CMB and Large-Scale Structure”,JCAP05(2014) 011,arXiv:1401.7597 [astro-ph.CO]

2014 arXiv
[252]

ETHOS – An Effective Theory of Structure Formation: From Dark Particle Physics to the Matter Distribution of the Universe

F.-Y. Cyr-Racine, K. Sigurdson, J. Zavala, T. Bringmann, M. Vogelsberger, and C. Pfrommer, “ETHOS – An Effective Theory of Structure Formation: From Dark Particle Physics to the Matter Distribution of the Universe”,Phys. Rev. D93(2016) 123527, arXiv:1512.05344 [astro-ph.CO]

2016 arXiv
[253]

Dark Matter-Neutrino Interactions through the Lens of Their Cosmological Implications

A. Olivares-Del Campo, C. Bœhm, S. Palomares-Ruiz, and S. Pascoli, “Dark Matter-Neutrino Interactions through the Lens of Their Cosmological Implications”,Phys. Rev. D97(2018) 075039, arXiv:1711.05283 [hep-ph]

2018 arXiv
[254]

Cosmological Probes of Dark Matter Interactions: The Next Decade

V. Gluscevic et al., “Cosmological Probes of Dark Matter Interactions: The Next Decade”,Bull. Am. Astron. Soc.51(2019) 134,arXiv:1903.05140 [astro-ph.CO]

2019 arXiv
[255]

The Full Boltzmann Hierarchy for Dark Matter-Massive Neutrino Interactions

M. Mosbech, C. Bœhm, S. Hannestad, O. Mena, J. Stadler, and Y. Y. Y. Wong, “The Full Boltzmann Hierarchy for Dark Matter-Massive Neutrino Interactions”,JCAP03(2021) 066, arXiv:2011.04206 [astro-ph.CO]

2021 arXiv
[256]

Snowmass2021 Theory Frontier White Paper: Astrophysical and Cosmological Probes of Dark Matter

K. Boddy et al., “Snowmass2021 Theory Frontier White Paper: Astrophysical and Cosmological Probes of Dark Matter”,JHEAp35(2022) 112,arXiv:2203.06380 [hep-ph]

2022 arXiv
[257]

Dark-Matter-Radiation Scattering Enhances CMB Phase Shift through Dark-Matter Loading

S. Ghosh, D. Ho, and Y. Tsai, “Dark-Matter-Radiation Scattering Enhances CMB Phase Shift through Dark-Matter Loading”,JCAP01(2025) 058,arXiv:2405.08064 [astro-ph.CO]

2025 arXiv
[258]

Asymmetric Dark Matter and Dark Radiation

M. Blennow, E. Fernandez-Martinez, O. Mena, J. Redondo, and P. Serra, “Asymmetric Dark Matter and Dark Radiation”,JCAP07(2012) 022,arXiv:1203.5803 [hep-ph]

2012 arXiv
[259]

Partially Acoustic Dark Matter, Interacting Dark Radiation, and Large-Scale Structure

Z. Chacko, Y. Cui, S. Hong, T. Okui, and Y. Tsai, “Partially Acoustic Dark Matter, Interacting Dark Radiation, and Large-Scale Structure”,JHEP12(2016) 108,arXiv:1609.03569 [astro-ph.CO]

2016 arXiv
[260]

Non-Perturbative Dynamics of Reheating after 65 Inflation: A Review

M. Amin, M. Hertzberg, D. Kaiser, and J. Karouby, “Non-Perturbative Dynamics of Reheating after 65 Inflation: A Review”,Int. J. Mod. Phys. D24(2014) 1530003,arXiv:1410.3808 [hep-ph]

2014 arXiv
[261]

Cosmological Backgrounds of Gravitational Waves

C. Caprini and D. Figueroa, “Cosmological Backgrounds of Gravitational Waves”,Class. Quant. Grav.35(2018) 163001,arXiv:1801.04268 [astro-ph.CO]

2018 arXiv
[262]

The First Three Seconds: A Review of Possible Expansion Histories of the Early Universe

R. Allahverdi et al., “The First Three Seconds: A Review of Possible Expansion Histories of the Early Universe”,Open J. Astrophys.4(2021) astro.2006.16182,arXiv:2006.16182 [astro-ph.CO]

2021 arXiv
[263]

Phase Transitions in the Early Universe

M. Hindmarsh, M. L¨ uben, J. Lumma, and M. Pauly, “Phase Transitions in the Early Universe”, SciPost Phys. Lect. Notes24(2021) 1,arXiv:2008.09136 [astro-ph.CO]

2021 arXiv
[264]

Detection of Early-Universe Gravitational-Wave Signatures and Fundamental Physics

R. Caldwell et al., “Detection of Early-Universe Gravitational-Wave Signatures and Fundamental Physics”,Gen. Rel. Grav.54(2022) 156,arXiv:2203.07972 [gr-qc]

2022 arXiv
[265]

Inflation: Theory and Observations

A. Ach´ ucarro et al., “Inflation: Theory and Observations”,arXiv:2203.08128 [astro-ph.CO]

arXiv
[266]

Cosmological Phase Transitions: From Perturbative Particle Physics to Gravitational Waves

P. Athron, C. Bal´ azs, A. Fowlie, L. Morris, and L. Wu, “Cosmological Phase Transitions: From Perturbative Particle Physics to Gravitational Waves”,Prog. Part. Nucl. Phys.135(2024) 104094, arXiv:2305.02357 [hep-ph]

2024 arXiv
[267]

Gravitational-Wave Experiments and Early-Universe Cosmology

M. Maggiore, “Gravitational-Wave Experiments and Early-Universe Cosmology”,Phys. Rept.331 (2000) 283,arXiv:gr-qc/9909001

2000 arXiv
[268]

A New Cosmic Microwave Background Constraint to Primordial Gravitational Waves

T. Smith, E. Pierpaoli, and M. Kamionkowski, “A New Cosmic Microwave Background Constraint to Primordial Gravitational Waves”,Phys. Rev. Lett.97(2006) 021301, arXiv:astro-ph/0603144

2006 arXiv
[269]

The NANOGrav 15-Year Data Set: Evidence for a Gravitational-Wave Background

G. Agazie et al. (NANOGrav Collaboration), “The NANOGrav 15-Year Data Set: Evidence for a Gravitational-Wave Background”,Astrophys. J. Lett.951(2023) L8,arXiv:2306.16213 [astro-ph.HE]

2023 arXiv
[270]

The Second Data Release from the European Pulsar Timing Array – III. Search for Gravitational-Wave Signals

J. Antoniadis et al. (EPTA and InPTA Collaborations), “The Second Data Release from the European Pulsar Timing Array – III. Search for Gravitational-Wave Signals”,Astron. Astrophys. 678(2023) A50,arXiv:2306.16214 [astro-ph.HE]

2023 arXiv
[271]

Search for an Isotropic Gravitational-Wave Background with the Parkes Pulsar Timing Array

D. Reardon et al., “Search for an Isotropic Gravitational-Wave Background with the Parkes Pulsar Timing Array”,Astrophys. J. Lett.951(2023) L6,arXiv:2306.16215 [astro-ph.HE]

2023 arXiv
[272]

Searching for the Nano-Hertz Stochastic Gravitational-Wave Background with the Chinese Pulsar Timing Array Data Release I

H. Xu et al., “Searching for the Nano-Hertz Stochastic Gravitational-Wave Background with the Chinese Pulsar Timing Array Data Release I”,Res. Astron. Astrophys.23(2023) 075024, arXiv:2306.16216 [astro-ph.HE]

2023 arXiv
[273]

The NANOGrav 15-Year Data Set: Constraints on Supermassive Black Hole Binaries from the Gravitational-Wave Background

G. Agazie et al. (NANOGrav Collaboration), “The NANOGrav 15-Year Data Set: Constraints on Supermassive Black Hole Binaries from the Gravitational-Wave Background”,Astrophys. J. Lett. 952(2023) L37,arXiv:2306.16220 [astro-ph.HE]

2023 arXiv
[274]

Does NANOGrav Observe a Dark-Sector Phase Transition?

T. Bringmann, P. F. Depta, T. Konstandin, K. Schmidt-Hoberg, and C. Tasillo, “Does NANOGrav Observe a Dark-Sector Phase Transition?”,JCAP11(2023) 053,arXiv:2306.09411 [astro-ph.CO]

2023 arXiv
[275]

The NANOGrav 15-Year Data Set: Search for Signals from New Physics

A. Afzal et al. (NANOGrav Collaboration), “The NANOGrav 15-Year Data Set: Search for Signals from New Physics”,Astrophys. J. Lett.951(2023) L11,arXiv:2306.16219 [astro-ph.HE]

2023 arXiv
[276]

What is the Source of the PTA GW Signal?

J. Ellis, M. Fairbairn, G. Franciolini, G. H¨ utsi, A. Iovino, M. Lewicki, M. Raidal, J. Urrutia, V. Vaskonen, and H. Veerm¨ ae, “What is the Source of the PTA GW Signal?”,Phys. Rev. D109 (2024) 023522,arXiv:2308.08546 [astro-ph.CO]

2024 arXiv
[277]

Disentangling the Origins of the NANOGrav Signal: Early-Universe Models and ∆N eff Bounds

I. Ben-Dayan, U. Kumar, and A. Verma, “Disentangling the Origins of the NANOGrav Signal: Early-Universe Models and ∆N eff Bounds”,JHEAp50(2026) 100510,arXiv:2508.15134 66 [astro-ph.CO]

2026
[278]

Multi-Wavelength Constraints on the Inflationary Consistency Relation

P. D. Meerburg, R. Hloˇ zek, B. Hadzhiyska, and J. Meyers, “Multi-Wavelength Constraints on the Inflationary Consistency Relation”,Phys. Rev. D91(2015) 103505,arXiv:1502.00302 [astro-ph.CO]

2015 arXiv
[279]

Gravitational-Wave Cosmology across 29 Decades in Frequency

P. Lasky et al., “Gravitational-Wave Cosmology across 29 Decades in Frequency”,Phys. Rev. X6 (2016) 011035,arXiv:1511.05994 [astro-ph.CO]

2016 arXiv
[280]

The Astrophysics of Nano-Hertz Gravitational Waves

S. Burke-Spolaor et al., “The Astrophysics of Nano-Hertz Gravitational Waves”,Astron. Astrophys. Rev.27(2019) 5,arXiv:1811.08826 [astro-ph.HE]

2019 arXiv
[281]

Upper Limits on the Isotropic Gravitational-Wave Background from Advanced LIGO and Advanced Virgo’s Third Observing Run

R. Abbott et al. (LIGO Scientific, Virgo and KAGRA Collaborations), “Upper Limits on the Isotropic Gravitational-Wave Background from Advanced LIGO and Advanced Virgo’s Third Observing Run”,Phys. Rev. D104(2021) 022004,arXiv:2101.12130 [gr-qc]

2021
[282]

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

A. Renzini, B. Goncharov, A. Jenkins, and P. Meyers, “Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects”,Galaxies10(2022) 34,arXiv:2202.00178 [gr-qc]

2022 arXiv
[283]

Cosmology with the Laser Interferometer Space Antenna

P. Auclair et al. (LISA Cosmology Working Group), “Cosmology with the Laser Interferometer Space Antenna”,Living Rev. Rel.26(2023) 5,arXiv:2204.05434 [astro-ph.CO]

2023 arXiv
[284]

MeV-Mass Dark Matter and Primordial Nucleosynthesis

P. Serpico and G. Raffelt, “ MeV-Mass Dark Matter and Primordial Nucleosynthesis”,Phys. Rev. D 70(2004) 043526,arXiv:astro-ph/0403417

2004 arXiv
[285]

Limits on MeV Dark Matter from the Effective Number of Neutrinos

C. M. Ho and R. Scherrer, “Limits on MeV Dark Matter from the Effective Number of Neutrinos”, Phys. Rev. D87(2013) 023505,arXiv:1208.4347 [astro-ph.CO]

2013 arXiv
[286]

A Lower Bound on the Mass of Cold Thermal Dark Matter from Planck

C. Bœhm, M. Dolan, and C. McCabe, “A Lower Bound on the Mass of Cold Thermal Dark Matter from Planck”,JCAP08(2013) 041,arXiv:1303.6270 [hep-ph]

2013 arXiv
[287]

BBN and the CMB Constrain Light, Electromagnetically Coupled WIMPs

K. Nollett and G. Steigman, “BBN and the CMB Constrain Light, Electromagnetically Coupled WIMPs”,Phys. Rev. D89(2014) 083508,arXiv:1312.5725 [astro-ph.CO]

2014 arXiv
[288]

BBN and the CMB Constrain Neutrino-Coupled Light WIMPs

K. Nollett and G. Steigman, “BBN and the CMB Constrain Neutrino-Coupled Light WIMPs”, Phys. Rev. D91(2015) 083505,arXiv:1411.6005 [astro-ph.CO]

2015 arXiv
[289]

The Cosmology of Sub-MeV Dark Matter

D. Green and S. Rajendran, “The Cosmology of Sub-MeV Dark Matter”,JHEP10(2017) 013, arXiv:1701.08750 [hep-ph]

2017 arXiv
[290]

Light Dark Matter: Models and Constraints

S. Knapen, T. Lin, and K. Zurek, “Light Dark Matter: Models and Constraints”,Phys. Rev. D96 (2017) 115021,arXiv:1709.07882 [hep-ph]

2017 arXiv
[291]

Neutrino Decoupling beyond the Standard Model: CMB Constraints on the Dark Matter Mass with a Fast and PreciseN eff Evaluation

M. Escudero, “Neutrino Decoupling beyond the Standard Model: CMB Constraints on the Dark Matter Mass with a Fast and PreciseN eff Evaluation”,JCAP02(2019) 007,arXiv:1812.05605 [hep-ph]

2019 arXiv
[292]

Refined Bounds on MeV-Scale Thermal Dark Sectors from BBN and the CMB

N. Sabti, J. Alvey, M. Escudero, M. Fairbairn, and D. Blas, “Refined Bounds on MeV-Scale Thermal Dark Sectors from BBN and the CMB”,JCAP01(2020) 004,arXiv:1910.01649 [hep-ph]

2020 arXiv
[293]

BBN Constraints on the Annihilation of MeV-Scale Dark Matter

P. Depta, M. Hufnagel, K. Schmidt-Hoberg, and S. Wild, “BBN Constraints on the Annihilation of MeV-Scale Dark Matter”,JCAP04(2019) 029,arXiv:1901.06944 [hep-ph]

2019 arXiv
[294]

Joint Cosmic Microwave Background and Big Bang Nucleosynthesis Constraints on Light Dark Sectors with Dark Radiation

C. Giovanetti, M. Lisanti, H. Liu, and J. Ruderman, “Joint Cosmic Microwave Background and Big Bang Nucleosynthesis Constraints on Light Dark Sectors with Dark Radiation”,Phys. Rev. Lett. 129(2022) 021302,arXiv:2109.03246 [hep-ph]

2022 arXiv
[295]

Toward a Full Description of MeV Dark Matter Decoupling: 67 A Self-Consistent Determination of Relic Abundance andN eff

X. Chu, J.-L. Kuo, and J. Pradler, “Toward a Full Description of MeV Dark Matter Decoupling: 67 A Self-Consistent Determination of Relic Abundance andN eff”,Phys. Rev. D106(2022) 055022, arXiv:2205.05714 [hep-ph]

2022 arXiv
[296]

What Does Cosmology Tell Us about the Mass of Thermal-Relic Dark Matter?

R. An, V. Gluscevic, E. Calabrese, and J. C. Hill, “What Does Cosmology Tell Us about the Mass of Thermal-Relic Dark Matter?”,JCAP07(2022) 002,arXiv:2202.03515 [astro-ph.CO]

2022 arXiv
[297]

Interacting Light Thermal-Relic Dark Matter: Self-Consistent Cosmological Bounds

R. An, K. Boddy, and V. Gluscevic, “Interacting Light Thermal-Relic Dark Matter: Self-Consistent Cosmological Bounds”,Phys. Rev. D109(2024) 123522,arXiv:2402.14223 [astro-ph.CO]

2024 arXiv
[298]

Freeze-In Production of FIMP Dark Matter

L. Hall, K. Jedamzik, J. March-Russell, and S. West, “Freeze-In Production of FIMP Dark Matter”, JHEP03(2010) 080,arXiv:0911.1120 [hep-ph]

2010 arXiv
[299]

Ultraviolet Freeze-In

F. Elahi, C. Kolda, and J. Unwin, “Ultraviolet Freeze-In”,JHEP03(2015) 048, arXiv:1410.6157 [hep-ph]

2015 arXiv
[300]

Chilly Dark Sectors and Asymmetric Reheating

P. Adshead, Y. Cui, and J. Shelton, “Chilly Dark Sectors and Asymmetric Reheating”,JHEP06 (2016) 016,arXiv:1604.02458 [hep-ph]

2016 arXiv

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.

[1] [72]

Raghunathan, C

S. Raghunathan, C. Trendafilova, J. Meyers, B. Wallisch et al., in preparation

[2] [1]

Snowmass Theory Frontier: Astrophysics and Cosmology

D. Green et al., “Snowmass Theory Frontier: Astrophysics and Cosmology”,arXiv:2209.06854 [hep-ph]

arXiv

[3] [2]

Report of the Topical Group on Cosmic Frontier 5 Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before for Snowmass 2021

C. Chang et al., “Report of the Topical Group on Cosmic Frontier 5 Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before for Snowmass 2021”,arXiv:2209.08265 [hep-ex]

arXiv 2021

[4] [3]

TASI Lectures on Cosmic Signals of Fundamental Physics

D. Green, “TASI Lectures on Cosmic Signals of Fundamental Physics”,PoSTASI2022(2024) 005, arXiv:2212.08685 [hep-ph]

arXiv 2024

[5] [4]

Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics

D. Green et al., “Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics”, Bull. Am. Astron. Soc.51(2019) 159,arXiv:1903.04763 [astro-ph.CO]

arXiv 2019

[6] [5]

Synergy between Cosmological and Laboratory Searches in Neutrino Physics

M. Gerbino et al., “Synergy between Cosmological and Laboratory Searches in Neutrino Physics”, Phys. Dark Univ.42(2023) 101333,arXiv:2203.07377 [hep-ph]

arXiv 2023

[7] [6]

The Physics of Light Relics

C. Dvorkin et al., “The Physics of Light Relics”,arXiv:2203.07943 [hep-ph]

arXiv

[8] [7]

Prospects and Limitations for Constraining Light Relics with Primordial Abundance Measurements

A. Lagu¨ e and J. Meyers, “Prospects and Limitations for Constraining Light Relics with Primordial Abundance Measurements”,Phys. Rev. D101(2020) 043509, arXiv:1908.05291 [astro-ph.CO]

arXiv 2020