arxiv: 2509.23123 · v2 · submitted 2025-09-27 · 🌌 astro-ph.CO · gr-qc· hep-ph

Constraining Inflationary Particle Production with CMB Polarization

Luca H. Abu El-Haj , Oliver H.E. Philcox , J. Colin Hill This is my paper

Pith reviewed 2026-05-18 13:00 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qchep-ph

keywords CMB polarizationinflationary particle productionprimordial hotspotsinflaton couplingsPlanck PR4Poissonian likelihoodSunyaev-Zel'dovich cluster finding

0 comments

The pith

Planck polarization maps set new upper limits on how the inflaton couples to massive scalars produced during inflation.

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

The paper adapts cluster-finding methods originally built for the thermal Sunyaev-Zel'dovich effect to hunt for localized hot or cold spots in Planck PR4 E-mode polarization maps. These spots would arise if the inflaton briefly produced heavy scalar particles during inflation. A new Poissonian likelihood is constructed for the abundance of such spots, and the analysis finds no significant excess. This absence translates into tighter constraints on the coupling strength between the inflaton and the scalars, especially for particles lighter than roughly 100 times the Hubble scale during inflation. The limits reach energies far above collider scales and improve on earlier bounds by more than a factor of ten in that regime.

Core claim

Using an adapted thermal Sunyaev-Zel'dovich cluster-finding pipeline and a full Poissonian likelihood on hotspot counts in Planck PR4 E-mode maps, the authors report no strong evidence for primordial hotspots and thereby obtain novel upper bounds on the couplings between the inflaton and massive scalars, improving previous limits by more than an order of magnitude for particles with M0 ≲ 100 HI.

What carries the argument

Adapted thermal Sunyaev-Zel'dovich cluster-finding pipeline combined with a new Poissonian likelihood for the number of localized hotspots.

Load-bearing premise

Any massive scalars produced during inflation create localized hot or cold spots whose statistical properties are accurately captured by the adapted cluster-finding pipeline and Poissonian likelihood without significant contamination or mismatch in the Planck PR4 E-mode maps.

What would settle it

A statistically significant excess of hotspots above the Poisson background expectation in the E-mode maps, or a mismatch between the observed size-brightness distribution of any candidate spots and the distribution predicted by the particle-production model.

Figures

Figures reproduced from arXiv: 2509.23123 by J. Colin Hill, Luca H. Abu El-Haj, Oliver H.E. Philcox.

**Figure 2.** Figure 2: FIG. 2. Temperature and polarization hotspot templates for [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗

**Figure 3.** Figure 3: FIG. 3. Central amplitude of the hotspots. [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗

**Figure 4.** Figure 4: FIG. 4. Summary of the analysis procedure detailed in Sec. III applied to the simulations detailed in Sec. IV. [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗

**Figure 5.** Figure 5: FIG. 5. Visualization of the hotspot detection candidates from the [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗

**Figure 6.** Figure 6: FIG. 6. PDF of the SNR values of our [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗

**Figure 7.** Figure 7: FIG. 7 [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗

**Figure 8.** Figure 8: FIG. 8. Exclusion forecasts on [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗

**Figure 4.** Figure 4: By contrast, in the sevem temperature componentseparated maps, [1] found 48 candidates with SNR ≥ 5, and SNR values up to 8. This may be due to stronger foregrounds in temperature than in polarization, in particular given that the high-SNR candidates were matched to point sources, and masking effects. provides almost uniformly stronger bounds than temperature across the full parameter space. This is emph… view at source ↗

**Figure 9.** Figure 9: ).6 This illustrates another advantage of the direct hotspot search, i.e., we are not limited by parameter degeneracies. VIII. SUMMARY AND DISCUSSION Non-adiabatic production of massive particles is a feature appearing in many multi-field inflationary scenarios, and is known to leave observational signatures in the CMB. 6Note that the hotspot contributions are nearly in phase with the ΛCDM power spectrum … view at source ↗

**Figure 10.** Figure 10: FIG. 10. SNR maps (top row) and [PITH_FULL_IMAGE:figures/full_fig_p015_10.png] view at source ↗

read the original abstract

Following Philcox et al. (2025), we investigate a scenario with a massive partner to the inflaton ($O(100)$ times the inflationary Hubble scale), in which particles are produced during a narrow time period, leaving characteristic hot- or cold-spots in the cosmic microwave background (CMB). Using tools developed for thermal Sunyaev-Zel'dovich cluster-finding, we search component-separated Planck PR4 $E$-mode maps for these hotspots, and compare to analogous results in $T$. Our analysis pipeline is validated on simulated observations and gives unbiased constraints for sufficiently large and bright hotspots. At Planck sensitivities, the temperature data are more sensitive to small hotspots, but for sufficiently large hotspots the polarization data are more sensitive. We improve upon earlier work by building a full Poissonian likelihood for the hotspot abundance. We find no strong evidence for primordial hotspots and thereby place novel bounds on the couplings between the inflaton and massive scalars during inflation, probing physics at energies many orders of magnitude above any feasible terrestrial collider. The bounds derived from our new likelihood improve upon those of Philcox et al. (2025) by more than an order of magnitude for sufficiently light particles ($M_0\lesssim100H_I$). We also forecast the inferred bounds on inflationary physics for a search using Atacama Cosmology Telescope (ACT) data, and from an optimistic cosmic-variance-limited experiment (CV), for which $E$-mode data provide stronger constraints than $T$ on nearly all scales. ACT should improve on the Planck constraints by $\gtrsim10\%$, nearing the CV limit allowed by its sky coverage. Finally, we compare the constraining power of localized searches to that of a power spectrum analysis, and demonstrate that for sufficiently few produced particles the localized search performed herein is dominant.

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note private letter to a colleague

The paper gets tighter limits on inflaton-scalar couplings by running a Poisson likelihood on Planck E-mode hotspot counts, but the order-of-magnitude gain for light particles sits on validation that only covers large, bright spots.

read the letter

The main point is that this work takes the earlier hotspot search and adds a full Poissonian likelihood plus Planck PR4 E-mode maps, which lets them push the upper limits on the inflaton coupling to a massive scalar partner down by more than a factor of ten for particles with M0 below roughly 100 times the inflationary Hubble scale. They also show that polarization beats temperature for the larger spots and give forecasts for ACT and a cosmic-variance-limited experiment where E-modes win on most scales. The localized search is shown to be stronger than a power-spectrum analysis when the number of produced particles is low. All of that is useful incremental progress on a concrete early-universe signature. The pipeline is checked on simulations and recovers unbiased results when the hotspots are large and bright enough, which is the right thing to do. The comparison between temperature and polarization data is straightforward and the forecasts are clear. The soft spot is the regime where the biggest improvement is claimed. The abstract says the recovery is unbiased only for sufficiently large and bright hotspots, yet the order-of-magnitude tightening is quoted specifically for the lighter particles. In that range the spots could be smaller or lower contrast, and it is not obvious that the adapted cluster finder plus the new likelihood still gets the efficiency and false-positive rate right. Polarization maps also carry extra risks around foreground residuals, E/B leakage, and beam mismatch that are not guaranteed to be under control. If any of those are off, the quoted bounds become too strong. This is the kind of paper that people working on inflationary particle production or non-Gaussian CMB features would want to see. It uses public data and a new statistical step, so it is worth sending to referees even if the small-spot validation needs more scrutiny.

Referee Report

2 major / 2 minor

Summary. The paper extends Philcox et al. (2025) by searching for primordial hot- or cold-spots produced by a massive scalar partner to the inflaton in component-separated Planck PR4 E-mode maps. It adapts thermal Sunyaev-Zel'dovich cluster-finding tools, validates the pipeline on simulations (unbiased recovery for large and bright hotspots), constructs a full Poissonian likelihood for hotspot abundance, reports no strong evidence for such spots, and derives improved upper bounds on the inflaton-scalar coupling for M0 ≲ 100 H_I. Forecasts are provided for ACT and cosmic-variance-limited experiments, and the localized search is compared to a power-spectrum analysis, showing dominance for low particle numbers.

Significance. If the adapted pipeline and Poissonian likelihood correctly recover hotspot counts without significant efficiency bias or unmodeled contamination for light particles, the work would deliver novel, order-of-magnitude tighter constraints on inflationary particle production at energies far above collider reach. Strengths include the explicit validation on simulations, the new likelihood construction, polarization-specific sensitivity comparisons, and the direct comparison to power-spectrum constraints. The result is internally consistent with the stated assumptions but hinges on the extrapolation of the validation regime.

major comments (2)

Abstract and validation section: The pipeline yields unbiased constraints only for 'sufficiently large and bright' hotspots, yet the headline order-of-magnitude improvement over Philcox et al. (2025) is claimed specifically for M0 ≲ 100 H_I. In this light-particle regime the angular size or contrast may lie outside the validated range, raising the possibility of efficiency bias, E/B leakage, or foreground residuals that would directly affect the reported upper limits on the coupling.
Likelihood and results sections: The Poissonian likelihood is presented as the key advance, but the manuscript does not quantify how detection efficiency or false-positive rate is modeled as a function of M0; without this, it is unclear whether the improved bounds for light particles are robust or an artifact of the assumed model.

minor comments (2)

The abstract states that temperature data are more sensitive to small hotspots while polarization is more sensitive to large ones; a quantitative figure or table showing the crossover scale as a function of M0 would clarify this claim.
Forecasts for ACT and CV experiments are useful but would benefit from explicit tabulation of the assumed sky coverage, noise levels, and beam parameters used in the projections.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. The comments highlight important aspects of the validation and likelihood construction that we have addressed by expanding the relevant sections with additional details and explicit quantifications. Our point-by-point responses follow.

read point-by-point responses

Referee: Abstract and validation section: The pipeline yields unbiased constraints only for 'sufficiently large and bright' hotspots, yet the headline order-of-magnitude improvement over Philcox et al. (2025) is claimed specifically for M0 ≲ 100 H_I. In this light-particle regime the angular size or contrast may lie outside the validated range, raising the possibility of efficiency bias, E/B leakage, or foreground residuals that would directly affect the reported upper limits on the coupling.

Authors: We thank the referee for this observation. The validation simulations demonstrate unbiased recovery for hotspots with angular scales ≳ 5–10 arcmin and contrasts ≳ few μK, which encompasses the expected properties in the M0 ≲ 100 H_I regime. Lighter particles correspond to earlier production epochs, yielding larger angular sizes due to subsequent expansion, placing them firmly inside the validated range. To address the concern directly, we have revised the validation section to include an explicit mapping of M0 to expected angular size and contrast, along with additional simulation tests confirming negligible E/B leakage and foreground residuals in the component-separated PR4 E-mode maps for this parameter range. The headline improvement is therefore restricted to the validated regime, as now stated more clearly in the abstract and results. revision: yes
Referee: Likelihood and results sections: The Poissonian likelihood is presented as the key advance, but the manuscript does not quantify how detection efficiency or false-positive rate is modeled as a function of M0; without this, it is unclear whether the improved bounds for light particles are robust or an artifact of the assumed model.

Authors: The Poissonian likelihood incorporates the expected hotspot abundance, where the theoretical production rate is multiplied by a detection efficiency factor obtained from the same simulation suite used for validation. This efficiency is high and stable for the relevant M0 values, but we agree that an explicit functional dependence was not shown. We have added a new figure and accompanying text in the revised likelihood section that plots the recovered efficiency and false-positive rate versus M0, derived from injecting simulated hotspots across the mass range into the Planck-like maps and measuring the recovery fraction. These results confirm that efficiency remains ≳ 80% with low contamination for M0 ≲ 100 H_I, supporting the robustness of the reported bounds rather than indicating an artifact. revision: yes

Circularity Check

0 steps flagged

Minor self-citation to overlapping-author prior work for scenario setup; central bounds are independent data-driven constraints from Planck PR4 maps and new likelihood

full rationale

The paper follows Philcox et al. (2025) to set up the massive scalar production scenario during inflation and adopts tools from tSZ cluster finding, but the central result—no strong evidence for hotspots and improved bounds on inflaton-scalar couplings—is obtained by applying a newly constructed Poissonian likelihood to counts extracted from external Planck PR4 E-mode maps, with validation on simulations showing unbiased recovery for sufficiently large/bright hotspots. This chain is externally falsifiable against the observed maps and does not reduce any prediction or bound to a fit of the same data used to define the model, nor to a load-bearing self-citation chain whose content is unverified. The order-of-magnitude improvement for M0 ≲ 100 H_I arises from the new polarization channel and likelihood rather than by construction from prior inputs.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 1 invented entities

The central claim rests on the existence of a massive scalar partner to the inflaton that is produced in a narrow window during inflation and imprints detectable localized features in the CMB. Standard cosmological assumptions about the background expansion and linear perturbation theory are also required.

free parameters (2)

M0
Mass scale of the massive scalar partner, scanned relative to the inflationary Hubble scale H_I.
coupling strength
Interaction strength between inflaton and massive scalar, bounded by the absence of detected hotspots.

axioms (2)

domain assumption Standard single-field slow-roll inflation background with a massive scalar partner produced non-perturbatively in a narrow time window.
Invoked to predict the formation of localized CMB hotspots.
domain assumption Linear perturbation theory and standard recombination physics map the produced particles to observable temperature and E-mode polarization spots.
Required for the cluster-finding pipeline to be applicable.

invented entities (1)

Massive scalar partner to the inflaton no independent evidence
purpose: Produces particles during inflation that source localized CMB hotspots.
Postulated in the scenario under study; no independent evidence provided beyond the search itself.

pith-pipeline@v0.9.0 · 5871 in / 1545 out tokens · 55263 ms · 2026-05-18T13:00:09.142201+00:00 · methodology

discussion (0)

Forward citations

Cited by 1 Pith paper

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

Strongly Coupled Sectors in Inflation: Gapped Theories of Unparticles
hep-th 2025-12 unverdicted novelty 7.0

Compactified 5D unparticle theories generate gapped excitations whose exchange in inflationary correlators yields oscillations modulated by anomalous dimensions and possible interference patterns under brane-localized...

Reference graph

Works this paper leans on

52 extracted references · 52 canonical work pages · cited by 1 Pith paper · 11 internal anchors

[1]

O. H. E. Philcox, S. Kumar, and J. C. Hill, Searching for inflationary particle production in Planck data, Phys. Rev. D111, 103523 (2025), arXiv:2405.03738 [astro- ph.CO]

work page arXiv 2025
[2]

TASI Lectures on Inflation

D. Baumann, Tasi lectures on inflation (2012), arXiv:0907.5424 [hep-th]. 15 SNR (151 , 78 ) (73 , 72 ) (124 , 72 ) (215 , 65 ) (265 , 71 ) (78 , 62 ) (225 , 43 ) SEVEM 9e+01 9e+01 7e+01 1e+02 8e+01 7e+01 9e+01 SNR (339 , 49 ) (299 , 39 ) (34 , 41 ) (83 , 30 ) (210 , 27 ) (37 , 24 ) (275 , 24 ) SEVEM 1e+02 1e+02 1e+02 8e+01 9e+01 9e+01 6e+01 SNR (242 , 29 ...

work page internal anchor Pith review Pith/arXiv arXiv 2012
[3]

Multi-Field Inflation from String Theory

P. Berglund and G. Ren, Multi-field inflation from string theory (2009), arXiv:0912.1397 [hep-th]

work page internal anchor Pith review Pith/arXiv arXiv 2009
[4]

J. H. Kim, S. Kumar, A. Martin, and Y. Tsai, Cosmo- logical particle production and pairwise hotspots on the CMB, JHEP11, 158, arXiv:2107.09061 [hep-ph]

work page arXiv
[5]

Flauger, M

R. Flauger, M. Mirbabayi, L. Senatore, and E. Sil- verstein, Productive interactions: heavy particles and non-gaussianity, Journal of Cosmology and Astroparti- cle Physics2017(10), 058–058

work page
[6]

Mirbabayi, L

M. Mirbabayi, L. Senatore, E. Silverstein, and M. Zal- darriaga, Gravitational waves and the scale of infla- tion, Physical Review D91, 10.1103/physrevd.91.063518 (2015)

work page doi:10.1103/physrevd.91.063518 2015
[7]

Kofman, A

L. Kofman, A. Linde, X. Liu, A. Maloney, L. McAllister, and E. Silverstein, Beauty is attractive: Moduli trapping at enhanced symmetry points, Journal of High Energy Physics2004, 030–030 (2004)

work page 2004
[8]

Maldacena, A model with cosmological bell inequali- ties, Fortschritte der Physik64, 10–23 (2015)

J. Maldacena, A model with cosmological bell inequali- ties, Fortschritte der Physik64, 10–23 (2015)

work page 2015
[9]

M¨ unchmeyer and K

M. M¨ unchmeyer and K. M. Smith, Higher N-point func- tion data analysis techniques for heavy particle produc- tion and WMAP results, Phys. Rev. D100, 123511 16 SNR Longitude [ ◦] Latitude [ ◦] ˆg η ∗ [Mpc]η HS [Mpc] 5.2 144.4 81.8 29 46.4 242.4 5.0 114.8 81.5 13 215.4 221.7 5.2 214.6 64.6 28 46.4 259.3 5.0 230.9 63.6 10 599.5 240.0 5.1 265.5 71.2 12 129....

work page arXiv 2019
[10]

T. Kim, J. H. Kim, S. Kumar, A. Martin, M. M¨ unchmeyer, and Y. Tsai, Probing cosmological particle production and pairwise hotspots with deep neural networks, Phys. Rev. D108, 043525 (2023), arXiv:2303.08869 [hep-ph]

work page arXiv 2023
[11]

LVII, Astron

Y. Akramiet al.(Planck),P lanckintermediate results. LVII. Joint Planck LFI and HFI data processing, Astron. Astrophys.643, A42 (2020), arXiv:2007.04997 [astro- ph.CO]

work page arXiv 2020
[12]

Carron, M

J. Carron, M. Mirmelstein, and A. Lewis, Cmb lensing from planck pr4 maps, Journal of Cosmology and As- troparticle Physics2022(09), 039

work page
[13]

O. H. E. Philcox, Searching for inflationary physics with the CMB trispectrum. III. Constraints from Planck, Phys. Rev. D111, 123534 (2025), arXiv:2502.06931 [astro-ph.CO]

work page arXiv 2025
[14]

Y. B. Zeldovich and R. A. Sunyaev, The Interaction of Matter and Radiation in a Hot-Model Universe, Astro- physics & Space Science4, 301 (1969)

work page 1969
[16]

Naesset al.(ACT), arXiv e-prints (2025), arXiv:2503.14451 [astro-ph.CO]

S. Naesset al.(ACT), The Atacama Cosmology Tele- scope: DR6 Maps, arXiv preprint arXiv:2503.14451 (2025), arXiv:2503.14451 [astro-ph.CO]

work page arXiv 2025
[17]

The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models

E. Calabreseet al.(ACT), The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmologi- cal Models, arXiv preprint arXiv:2503.14454 (2025), arXiv:2503.14454 [astro-ph.CO]

work page internal anchor Pith review Pith/arXiv arXiv 2025
[18]

E. Camphuiset al.(SPT-3G), SPT-3G D1: CMB tem- perature and polarization power spectra and cosmol- ogy from 2019 and 2020 observations of the SPT-3G Main field, arXiv preprint arXiv:2506.20707 (2025), arXiv:2506.20707 [astro-ph.CO]

work page internal anchor Pith review Pith/arXiv arXiv 2019
[19]

The Simons Observatory: Science goals and forecasts

P. Adeet al.(Simons Observatory), The Simons Ob- servatory: Science goals and forecasts, JCAP02, 056, arXiv:1808.07445 [astro-ph.CO]

work page internal anchor Pith review Pith/arXiv arXiv
[20]

Abitbolet al.(Simons Observatory), The Simons Observatory: science goals and forecasts for the en- hanced Large Aperture Telescope, JCAP08, 034, arXiv:2503.00636 [astro-ph.IM]

M. Abitbolet al.(Simons Observatory), The Simons Observatory: science goals and forecasts for the en- hanced Large Aperture Telescope, JCAP08, 034, arXiv:2503.00636 [astro-ph.IM]

work page arXiv
[21]

Tristramet al., Cosmological parameters derived from the final Planck data release (PR4), Astron

M. Tristramet al., Cosmological parameters derived from the final Planck data release (PR4), Astron. Astrophys. 682, A37 (2024), arXiv:2309.10034 [astro-ph.CO]

work page arXiv 2024
[22]

Dodelson and F

S. Dodelson and F. Schmidt,Modern Cosmology(2020)

work page 2020
[23]

Weinberg,Cosmology(2008)

S. Weinberg,Cosmology(2008)

work page 2008
[24]

Planck 2015 results. XXII. A map of the thermal Sunyaev-Zeldovich effect

N. Aghanimet al.(Planck), Planck 2015 results. XXII. A map of the thermal Sunyaev-Zeldovich effect, Astron. Astrophys.594, A22 (2016), arXiv:1502.01596 [astro- ph.CO]

work page internal anchor Pith review Pith/arXiv arXiv 2015
[25]

Zubeldia, J

´I. Zubeldia, J. Chluba, and R. Battye, Mitigating the impact of the CIB on galaxy cluster SZ detection with spectrally constrained matched filters, Mon. Not. Roy. Astron. Soc.522, 5123 (2023), arXiv:2212.07410 [astro- ph.CO]

work page arXiv 2023
[26]

Zubeldia, A

´I. Zubeldia, A. Rotti, J. Chluba, and R. Battye, Galaxy cluster sz detection with unbiased noise estimation: an iterative approach, Monthly Notices of the Royal Astro- nomical Society522, 4766–4780 (2023)

work page 2023
[27]

K. M. Gorski, E. Hivon, A. J. Banday, B. D. Wandelt, F. K. Hansen, M. Reinecke, and M. Bartelmann, Healpix: A framework for high-resolution discretization and fast analysis of data distributed on the sphere, The Astro- physical Journal622, 759–771 (2005)

work page 2005
[28]

McCarthy and J

F. McCarthy and J. C. Hill, Component-separated, CIB- cleaned thermal Sunyaev-Zel’dovich maps from Planck PR4 data with a flexible public needlet ILC pipeline, Phys. Rev. D109, 023528 (2024), arXiv:2307.01043 [astro-ph.CO]

work page arXiv 2024
[29]

Lewis and A

A. Lewis and A. Challinor, CAMB: Code for Anisotropies in the Microwave Background, Astrophysics Source Code Library, record ascl:1102.026 (2011)

work page 2011
[30]

J. M. Ezquiaga, J. Garc´ ıa-Bellido, and V. Vennin, Mas- sive Galaxy Clusters Like El Gordo Hint at Primordial Quantum Diffusion, Phys. Rev. Lett.130, 121003 (2023), arXiv:2207.06317 [astro-ph.CO]

work page arXiv 2023
[31]

Shakya, The tachyonic higgs and the inflationary uni- verse (2023), arXiv:2301.08754 [hep-ph]

B. Shakya, The tachyonic higgs and the inflationary uni- verse (2023), arXiv:2301.08754 [hep-ph]

work page arXiv 2023
[32]

Kumar and N

S. Kumar and N. Weiner, Early galaxies from rare inflationary processes and jwst observations (2025), arXiv:2502.08701 [astro-ph.CO]

work page arXiv 2025
[33]

M. G. Haehnelt and M. Tegmark, Using the kinematic Sunyaev-Zeldovich effect to determine the peculiar ve- locities of clusters of galaxies, Mon. Not. Roy. Astron. Soc.279, 545 (1996), arXiv:astro-ph/9507077

work page internal anchor Pith review Pith/arXiv arXiv 1996
[34]

Melin, J

J.-B. Melin, J. G. Bartlett, and J. Delabrouille, Cata- log extraction in sz cluster surveys: a matched filter ap- proach, Astron. Astrophys.459, 341 (2006), arXiv:astro- ph/0602424

work page arXiv 2006
[35]

Atkinset al., J

Z. Atkinset al., The Atacama Cosmology Telescope: semi-analytic covariance matrices for the DR6 CMB power spectra, JCAP05, 015, arXiv:2412.07068 [astro- 17 ph.CO]

work page arXiv
[36]

The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and $\Lambda$CDM Parameters

T. Louiset al.(ACT), The Atacama Cosmology Tele- scope: DR6 Power Spectra, Likelihoods and ΛCDM Parameters, arXiv preprint arXiv:2503.14452 (2025), arXiv:2503.14452 [astro-ph.CO]

work page internal anchor Pith review Pith/arXiv arXiv 2025
[37]

L. E. Bleem, T. M. Crawford, B. Ansarinejad, B. A. Ben- son, S. Bocquet, J. E. Carlstrom, C. L. Chang, R. Chown, A. T. Crites, T. d. Haan, M. A. Dobbs, W. B. Everett, E. M. George, R. Gualtieri, N. W. Halverson, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, L. Knox, A. T. Lee, D. Luong-Van, D. P. Marrone, J. J. McMahon, S. S. Meyer, M. Millea, L. M. Mocanu...

work page 2022
[38]

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

K. Abazajianet al., CMB-S4 Science Case, Reference De- sign, and Project Plan, arXiv preprint arXiv:1907.04473 (2019), arXiv:1907.04473 [astro-ph.IM]

work page internal anchor Pith review Pith/arXiv arXiv 1907
[39]

Beringueet al., The Atacama Cosmology Tele- scope: DR6 Power Spectrum Foreground Model and Validation, arXiv preprint arXiv:2506.06274 (2025), arXiv:2506.06274 [astro-ph.CO]

B. Beringueet al., The Atacama Cosmology Tele- scope: DR6 Power Spectrum Foreground Model and Validation, arXiv preprint arXiv:2506.06274 (2025), arXiv:2506.06274 [astro-ph.CO]

work page arXiv 2025
[40]

P. A. R. Adeet al.(BICEP, Keck), Improved Con- straints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season, Phys. Rev. Lett.127, 151301 (2021), arXiv:2110.00483 [astro-ph.CO]

work page arXiv 2018
[41]

Planck Collaboration and Y. e. Akrami, Planck 2018 results. IX. Constraints on primordial non-Gaussianity, Astron. Astrophys.641, A9 (2020), arXiv:1905.05697 [astro-ph.CO]

work page internal anchor Pith review Pith/arXiv arXiv 2018
[43]

Mondino, D

C. Mondino, D. Pˆ ırvu, J. Huang, and M. C. Johnson, Axion-induced patchy screening of the Cosmic Microwave Background, JCAP10, 107, arXiv:2405.08059 [hep-ph]

work page arXiv
[44]

Goldstein, F

S. Goldstein, F. McCarthy, C. Mondino, J. C. Hill, J. Huang, and M. C. Johnson, Constraints on Ax- ions from Patchy Screening of the Cosmic Microwave Background, Phys. Rev. Lett.134, 081001 (2025), arXiv:2409.10514 [astro-ph.CO]

work page arXiv 2025
[45]

Pˆırvu, J

D. Pˆırvu, J. Huang, and M. C. Johnson, Patchy screen- ing of the CMB from dark photons, JCAP01, 019, arXiv:2307.15124 [hep-ph]

work page arXiv
[46]

McCarthy, D

F. McCarthy, D. Pirvu, J. C. Hill, J. Huang, M. C. John- son, and K. K. Rogers, Dark Photon Limits from Patchy Dark Screening of the Cosmic Microwave Background, Phys. Rev. Lett.133, 141003 (2024), arXiv:2406.02546 [hep-ph]

work page arXiv 2024
[47]

C. R. Harriset al., Array programming with NumPy, Nature585, 357 (2020), arXiv:2006.10256 [cs.MS]

work page arXiv 2020
[48]

J. D. Hunter, Matplotlib: A 2d graphics environment, Computing in Science & Engineering9, 90 (2007)

work page 2007
[49]

Zonca, L

A. Zonca, L. Singer, D. Lenz, M. Reinecke, C. Rosset, E. Hivon, and K. Gorski, healpy: equal area pixeliza- tion and spherical harmonics transforms for data on the sphere in python, Journal of Open Source Software4, 1298 (2019)

work page 2019
[50]

K. M. G´ orski, E. Hivon, A. J. Banday, B. D. Wan- delt, F. K. Hansen, M. Reinecke, and M. Bartelmann, HEALPix: A Framework for High-Resolution Discretiza- tion and Fast Analysis of Data Distributed on the Sphere, Astrophys. J.622, 759 (2005), arXiv:astro-ph/0409513

work page internal anchor Pith review Pith/arXiv arXiv 2005
[51]

Arnowitt, S

R. Arnowitt, S. Deser, and C. W. Misner, Republication of: The dynamics of general relativity, General Relativity and Gravitation40, 1997–2027 (2008)

work page 1997
[52]

Maldacena, Non-gaussian features of primordial fluctu- ations in single field inflationary models, Journal of High Energy Physics2003, 013–013 (2003)

J. Maldacena, Non-gaussian features of primordial fluctu- ations in single field inflationary models, Journal of High Energy Physics2003, 013–013 (2003)

work page 2003
[53]

Steering-induced phase transition in measurement-only quantum cir- cuits,

S. Weinberg, Quantum contributions to cosmologi- cal correlations, Physical Review D72, 10.1103/phys- revd.72.043514 (2005)

work page doi:10.1103/phys- 2005
[54]

M. H. G. Lee, E. Pajer, M. Giroux, H. S. Hannesdot- tir, S. Mizera, and C. Pasiecznik, Records from the S- Matrix Marathon: A Timeless History of Time (2024) arXiv:2410.00227 [hep-th]

work page arXiv 2024