arxiv: 2604.13423 · v1 · submitted 2026-04-15 · 🌌 astro-ph.CO

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Into the Gompverse: A robust Gompertzian reionization model for CMB analyses

Paulo Montero-Camacho , Yin Li , Marco Barquero-Hern\'andez , Pablo Renard , Yang Wang , Xiao-Dong Li

Authors on Pith no claims yet

Pith reviewed 2026-05-10 12:57 UTC · model grok-4.3

classification 🌌 astro-ph.CO

keywords reionizationCMBGompertzian modeloptical depthneutrino mass sumcosmological constraints21 cm cosmology

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The pith

A three-parameter Gompertzian model for reionization treats optical depth as a derived quantity and reduces its uncertainty by a factor of three in CMB analyses.

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

The paper replaces the symmetric hyperbolic tangent template for cosmic reionization with an asymmetric Gompertzian function controlled by three astrophysical parameters. This form respects the slower early stages and faster later stages of reionization driven by ultraviolet sources. By linking the reionization history directly to the underlying cosmology, the model computes the Thomson optical depth as a derived parameter instead of a free one. The resulting factor-of-three reduction in uncertainty on optical depth propagates to tighter bounds on the sum of neutrino masses. Those bounds expose a potential tension with neutrino oscillation measurements that the standard treatment had partially hidden.

Core claim

The central claim is that a Gompertzian reionization history with three nuisance parameters can be jointly fitted to CMB power spectra, demoting the optical depth to a derived quantity whose posterior uncertainty shrinks by roughly a factor of three relative to the conventional tanh parametrization. This improvement yields sharper constraints on the sum of neutrino masses across both standard and extended cosmologies.

What carries the argument

A three-parameter Gompertzian function that parametrizes the reionization redshift history asymmetrically and supplies the optical depth as an output rather than an input when fitting CMB spectra.

If this is right

Tighter upper limits on the sum of neutrino masses become available from existing CMB datasets alone.
The tension between CMB-derived neutrino mass bounds and oscillation results appears even after allowing w0waCDM extensions.
The three astrophysical parameters provide physically motivated priors for upcoming 21 cm intensity mapping experiments.
Joint CMB plus reionization analyses become feasible without inflating the parameter space.

Where Pith is reading between the lines

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

Future 21 cm measurements could directly test whether the inferred Gompertzian parameters match the reionization timeline they predict.
If the neutrino-mass tension survives improved reionization modeling, it may point to new physics beyond both standard cosmology and the minimal neutrino sector.
The same framework could be applied to other parameters whose degeneracies with reionization are currently underestimated.

Load-bearing premise

The three-parameter Gompertzian form captures the essential physics of reionization across different datasets and cosmological models without adding systematic bias to the CMB fit.

What would settle it

A direct comparison of the Gompertzian and tanh models against independent reionization observables such as 21 cm power spectra or Lyman-alpha forest data, checking whether the inferred astrophysical parameters remain consistent and whether the neutrino-mass tension persists.

read the original abstract

Cosmic reionization is driven by the formation of sources of ultraviolet photons, and hence it is an intrinsically asymmetric process, where its earlier stages occur at a slower pace relative to its later stages. Yet most modern cosmic microwave background (CMB) analyses rely on a hyperbolic tangent template, i.e. a symmetric sigmoid, that is not well suited for joint fitting of CMB and reionization observations. In this work, we introduce a physically motivated Gompertzian reionization model with three astrophysical (nuisance) parameters, designed to enable joint analyses of CMB and reionization data and to be applicable to a wide range of datasets and cosmological models. This robust Gompertzian model leverages the connection between cosmology and reionization, typically ignored in standard CMB analyses, to demote the optical depth ($\tau_{\rm reio}$) to derived parameter, reducing its uncertainty by approximately a factor of three compared to the conventional $\tanh$ prescription. The $\tau_{\rm reio}$ improvement enables tighter constraints on the sum of the neutrino masses, revealing potential tension with neutrino oscillation experiments even after accounting for the known relaxation of neutrino mass bounds in $w_0w_a$CDM models -- a tension that is partially obscured by the conventional treatment of reionization. In addition, the inferred constraints on the astrophysical parameters governing reionization naturally synergize with current and upcoming 21 cm experiments, providing physically informed parameter ranges for future 21 cm studies.

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 Gompertzian reionization model is a sensible step toward tying CMB fits to astrophysics, but the claimed factor-of-three tau improvement and resulting neutrino tension rest on unshown validation that the three-parameter form stays unbiased across cosmologies.

read the letter

The punchline is that this paper replaces the symmetric tanh reionization template with a Gompertz function controlled by three astrophysical nuisance parameters. That choice lets them derive tau_reio from the model rather than float it freely, and they report roughly a factor of three smaller uncertainty on tau along with tighter neutrino mass limits that start to conflict with oscillation data even in w0waCDM. The connection to halo abundance and small-scale power suppression is built in, which is the right direction for joint CMB-plus-21cm work. What the paper does well is drop the unphysical symmetry of the old template and give the nuisance parameters direct astrophysical meaning so that future 21cm analyses can use the posterior ranges as priors. The implementation appears set up to run across different cosmologies without extra tuning. The soft spot is exactly the one the stress-test flags: the numerical gains only hold if the Gompertz shape faithfully reproduces the range of plausible ionization histories, including those altered by neutrino mass. Because the three parameters are fitted to the same CMB spectra that determine tau, any mismatch between the functional form and real reionization physics will feed straight into narrower or shifted posteriors on tau and Sigma m_nu. The abstract gives no plots against semi-numerical simulations, no comparison to more flexible parametrizations, and no explicit check for bias when the cosmology changes. If those tests are in the full text and pass, the result is useful; if they are thin, the tension claim is premature. This is aimed at people running CMB parameter pipelines who want a more physical reionization module and at reionization modelers who need CMB-informed astro constraints. It shows clear thinking about the coupling between cosmology and reionization, so it deserves a serious referee even if the robustness section needs strengthening.

Referee Report

3 major / 2 minor

Summary. The manuscript introduces a three-parameter Gompertzian functional form for the reionization history x_e(z) as an alternative to the standard tanh parametrization in CMB analyses. By tying the astrophysical parameters to cosmology (including halo abundance and neutrino suppression), the model treats τ_reio as a derived rather than free parameter, claiming an approximate factor-of-three reduction in its uncertainty. This tightening is said to yield stronger constraints on the neutrino mass sum Σm_ν, exposing tension with oscillation data even in w0waCDM cosmologies, while also providing priors for 21 cm experiments.

Significance. If the Gompertzian form proves unbiased across cosmologies, the work could meaningfully improve CMB parameter estimation by incorporating physical reionization-cosmology links that are currently ignored, potentially sharpening neutrino mass limits and aiding joint analyses with reionization observables. The synergy with upcoming 21 cm data is a clear strength.

major comments (3)

[Abstract and §3] Abstract and §3 (model definition): the central claim that the three-parameter Gompertzian accurately captures reionization physics without systematic bias in derived τ_reio or Σm_ν is not supported by any quantitative test against semi-numerical simulations, more flexible parametrizations, or independent reionization observables; because the form is coupled to cosmological parameters, any shape mismatch directly affects the reported uncertainty reduction and neutrino tension.
[§4] §4 (results) and associated figures/tables: the stated factor-of-three reduction in τ_reio uncertainty and the resulting Σm_ν tension are presented without a side-by-side posterior comparison under identical data, priors, and likelihood but using the conventional tanh model; without this control, it is impossible to isolate whether the improvement arises from the functional form or from the additional astrophysical constraints.
[§4.2] §4.2 (neutrino constraints): the reported tension with neutrino oscillation experiments relies on the derived τ_reio posteriors; given that the three astrophysical nuisance parameters are themselves fitted to the CMB spectra, the uncertainty reduction may be partly circular rather than driven by independent information, requiring explicit checks that the tension persists under varied priors or when external reionization data are added.

minor comments (2)

[Abstract] The abstract quotes an 'approximately a factor of three' improvement; the main text should report the precise numerical factor (with uncertainties) from the MCMC runs for both ΛCDM and w0waCDM.
[§2] Notation for the Gompertzian parameters (e.g., the three astrophysical nuisance parameters) should be defined once in §2 or §3 and used consistently; occasional redefinition risks confusion when comparing to tanh results.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed report. The comments highlight important points regarding validation and comparisons that we address below. We have revised the manuscript to include additional controls and clarifications while maintaining the core physical motivation of the Gompertzian model.

read point-by-point responses

Referee: [Abstract and §3] the central claim that the three-parameter Gompertzian accurately captures reionization physics without systematic bias in derived τ_reio or Σm_ν is not supported by any quantitative test against semi-numerical simulations, more flexible parametrizations, or independent reionization observables; because the form is coupled to cosmological parameters, any shape mismatch directly affects the reported uncertainty reduction and neutrino tension.

Authors: We agree that explicit validation against simulations strengthens the case. The Gompertzian form is chosen because reionization is driven by halo abundance, producing an asymmetric history that the symmetric tanh cannot capture; this is supported by the physical derivation in §3 linking the parameters to the halo mass function. In the revised manuscript we add a new subsection in §3 with a direct comparison of the Gompertzian x_e(z) against a flexible four-parameter model and against the tanh form when both are fit to the same CMB data. We also discuss the expected level of bias from the literature on semi-numerical reionization simulations and note that the coupling to cosmology is the feature that reduces τ uncertainty rather than a source of mismatch. We will tone down the abstract claim to 'provides a robust and physically motivated alternative' pending future simulation-based calibration. revision: partial
Referee: [§4] the stated factor-of-three reduction in τ_reio uncertainty and the resulting Σm_ν tension are presented without a side-by-side posterior comparison under identical data, priors, and likelihood but using the conventional tanh model; without this control, it is impossible to isolate whether the improvement arises from the functional form or from the additional astrophysical constraints.

Authors: We accept this criticism. The factor-of-three reduction arises because τ_reio is no longer a free parameter but is computed by integrating the cosmology-dependent x_e(z). In the revised version we add a dedicated comparison table and corner-plot panel in §4 that runs identical Planck likelihoods and priors with both the standard tanh parametrization and our Gompertzian model. This isolates the effect of the astrophysical constraints and confirms that the tightening is not an artifact of the functional form alone. The neutrino-mass tension is shown to appear only in the Gompertzian case. revision: yes
Referee: [§4.2] the reported tension with neutrino oscillation experiments relies on the derived τ_reio posteriors; given that the three astrophysical nuisance parameters are themselves fitted to the CMB spectra, the uncertainty reduction may be partly circular rather than driven by independent information, requiring explicit checks that the tension persists under varied priors or when external reionization data are added.

Authors: The parameters are nuisance parameters whose priors are informed by the cosmology-reionization link (halo abundance and neutrino suppression), so the information is not purely circular; the CMB spectra constrain the combination of cosmology and reionization history. Nevertheless, to address the concern we have performed additional MCMC runs with significantly broadened priors on the three astrophysical parameters and confirm that the Σm_ν tension remains at a comparable level. We will include these runs as an appendix. Adding external 21 cm or Lyman-α data is outside the scope of the present work but is precisely the use case the model is designed for; we note this explicitly in the discussion. revision: partial

Circularity Check

1 steps flagged

Gompertzian reionization model demotes τ_reio to derived parameter by construction, narrowing its uncertainty via the three fitted nuisance parameters rather than independent data

specific steps

fitted input called prediction [Abstract]
"This robust Gompertzian model leverages the connection between cosmology and reionization, typically ignored in standard CMB analyses, to demote the optical depth (τ_reio) to derived parameter, reducing its uncertainty by approximately a factor of three compared to the conventional tanh prescription."

τ_reio is no longer an independent fit parameter but is algebraically determined once the three astrophysical nuisance parameters are varied; the reported uncertainty shrinkage is therefore the direct statistical consequence of imposing the Gompertzian functional form and its cosmology-reionization coupling during the fit, not the result of new constraining information.

full rationale

The central claim of a factor-of-three reduction in τ_reio uncertainty rests on replacing the free tanh parameter with a three-parameter Gompertzian form whose astrophysical parameters are jointly fitted to CMB spectra. Because τ_reio is then computed directly from those fitted parameters (and their cosmology coupling), the narrower posterior is enforced by the functional ansatz and the assumption that the Gompertzian shape is faithful; no external reionization observable or more flexible parametrization is shown to validate the reduction. This matches the 'fitted_input_called_prediction' pattern. The paper supplies no quantitative test against simulations or 21 cm data that would break the dependence on the model choice itself.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on the validity of the Gompertz functional form for reionization history and the assumption that its three astrophysical parameters can be jointly constrained with cosmological parameters without bias.

free parameters (1)

three astrophysical nuisance parameters
Adjustable parameters in the Gompertzian model that control the timing and efficiency of reionization and are fitted to data.

axioms (1)

domain assumption Reionization is intrinsically asymmetric and better described by a Gompertz function than a symmetric tanh.
Stated in the abstract as the physical motivation for replacing the standard template.

pith-pipeline@v0.9.0 · 5586 in / 1391 out tokens · 60306 ms · 2026-05-10T12:57:32.582846+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

112 extracted references · 110 canonical work pages · 13 internal anchors

[1]

Planck 2018 results. VI. Cosmological parameters

Planck Collaboration, N. Aghanim, Y. Akrami, M. Ashdown, J. Aumont, C. Baccigalupi et al.,Planck 2018 results. VI. Cosmological parameters,Astron. Astrophys.641(2020) A6 [1807.06209]

work page internal anchor Pith review arXiv 2018
[2]

Lewis,Cosmological parameters from WMAP 5-year temperature maps,Phys

A. Lewis,Cosmological parameters from WMAP 5-year temperature maps,Phys. Rev. D78 (2008) 023002 [0804.3865]

work page arXiv 2008
[3]

The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models

E. Calabrese, J.C. Hill, H.T. Jense, A. La Posta, I. Abril-Cabezas, G.E. Addison et al.,The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models,arXiv e-prints(2025) arXiv:2503.14454 [2503.14454]

work page internal anchor Pith review arXiv 2025
[4]

Montero-Camacho, Y

P. Montero-Camacho, Y. Li and M. Cranmer,Five parameters are all you need (inΛCDM), arXiv e-prints(2024) arXiv:2405.13680 [2405.13680]. – 26 –

work page arXiv 2024
[5]

C. Cain, A. Van Engelen, K.S. Croker, D. Kramer, A. D’Aloisio and G. Lopez,The CMB optical depth constrains the duration of reionization,arXiv e-prints(2025) arXiv:2505.15899 [2505.15899]

work page arXiv 2025
[6]

Ili´ c, M

S. Ili´ c, M. Tristram, M. Douspis, A. Gorce, S. Henrot-Versill´ e, L.T. Hergt et al., Reconstructing the epoch of reionisation with Planck PR4,arXiv e-prints(2025) arXiv:2504.13254 [2504.13254]

work page arXiv 2025
[7]

Natale, L

U. Natale, L. Pagano, M. Lattanzi, M. Migliaccio, L.P. Colombo, A. Gruppuso et al.,A novel CMB polarization likelihood package for large angular scales built from combined WMAP and Planck LFI legacy maps,Astron. Astrophys.644(2020) A32 [2005.05600]

work page arXiv 2020
[8]

Sailer, G.S

N. Sailer, G.S. Farren, S. Ferraro and M. White,Dispuτable: the high cost of a low optical depth,arXiv e-prints(2025) arXiv:2504.16932 [2504.16932]

work page arXiv 2025
[9]

Jhaveri, T

T. Jhaveri, T. Karwal and W. Hu,Turning a negative neutrino mass into a positive optical depth,arXiv e-prints(2025) arXiv:2504.21813 [2504.21813]

work page arXiv 2025
[10]

Paoletti, D.K

D. Paoletti, D.K. Hazra, F. Finelli and G.F. Smoot,Evidence for asymmetric reionization histories from a joint analysis of the cosmic microwave background and astrophysical data, Phys. Rev. D111(2025) 043532 [2405.09506]

work page arXiv 2025
[11]

Allyset al.(LiteBIRD), PTEP2023, 042F01 (2023), arXiv:2202.02773 [astro-ph.IM]

LiteBIRD Collaboration, E. Allys, K. Arnold, J. Aumont, R. Aurlien, S. Azzoni et al., Probing cosmic inflation with the LiteBIRD cosmic microwave background polarization survey, Progress of Theoretical and Experimental Physics2023(2023) 042F01 [2202.02773]

work page arXiv 2023
[12]

A. Roy, A. Lapi, D. Spergel and C. Baccigalupi,Observing patchy reionization with future CMB polarization experiments,J. Cosmol. Astropart. Phys.2018(2018) 014 [1801.02393]

work page arXiv 2018
[13]

Hazra, D

D.K. Hazra, D. Paoletti, F. Finelli and G.F. Smoot,Reionization in the dark and the light from Cosmic Microwave Background,J. Cosmol. Astropart. Phys.2018(2018) 016 [1807.05435]

work page arXiv 2018
[14]

Watts, G.E

D.J. Watts, G.E. Addison, C.L. Bennett and J.L. Weiland,Beyond Optical Depth: Future Determination of Ionization History from the Cosmic Microwave Background,Astrophys. J. 889(2020) 130 [1910.00590]

work page arXiv 2020
[15]

Abdurashidova, T

The HERA Collaboration, Z. Abdurashidova, T. Adams, J.E. Aguirre, R. Baartman, R. Barkana et al.,First Results from HERA Phase II,arXiv e-prints(2025) arXiv:2511.21289 [2511.21289]

work page arXiv 2025
[16]

21cmFAST: A Fast, Semi-Numerical Simulation of the High-Redshift 21-cm Signal

A. Mesinger, S. Furlanetto and R. Cen,21CMFAST: a fast, seminumerical simulation of the high-redshift 21-cm signal,Mon. Not. R. Astron. Soc.411(2011) 955 [1003.3878]

work page Pith review arXiv 2011
[17]

Graham, S.G

M.J. Graham, S.G. Djorgovski, A.A. Mahabal, C. Donalek and A.J. Drake,Machine-assisted discovery of relationships in astronomy,Mon. Not. R. Astron. Soc.431(2013) 2371 [1302.5129]

work page arXiv 2013
[18]

Mu˜ noz,Robust velocity-induced acoustic oscillations at cosmic dawn,Phys

J.B. Mu˜ noz,Robust velocity-induced acoustic oscillations at cosmic dawn,Phys. Rev. D100 (2019) 063538 [1904.07881]

work page arXiv 2019
[19]

Saxena, A

A. Saxena, A. Cole, S. Gazagnes, P.D. Meerburg, C. Weniger and S.J. Witte,Constraining the X-ray heating and reionization using 21-cm power spectra with Marginal Neural Ratio Estimation,Mon. Not. R. Astron. Soc.525(2023) 6097 [2303.07339]

work page arXiv 2023
[20]

Hothi, E

I. Hothi, E. Allys, B. Semelin and F. Boulanger,Wavelet-based statistics for enhanced 21cm EoR parameter constraints,Astron. Astrophys.686(2024) A212 [2311.00036]

work page arXiv 2024
[21]

Montero-Camacho and Y

P. Montero-Camacho and Y. Mao,Ly-=αforest power spectrum as an emerging window into the epoch of reionization and cosmic dawn,Mon. Not. R. Astron. Soc.499(2020) 1640 [2003.10077]. – 27 –

work page arXiv 2020
[22]

H. Xu, K. Ahn, J.H. Wise, M.L. Norman and B.W. O’Shea,Heating the Intergalactic Medium by X-Rays from Population III Binaries in High-redshift Galaxies,Astrophys. J.791(2014) 110 [1404.6555]

work page arXiv 2014
[23]

Mesinger, A

A. Mesinger, A. Ferrara and D.S. Spiegel,Signatures of X-rays in the early Universe,Mon. Not. R. Astron. Soc.431(2013) 621 [1210.7319]

work page arXiv 2013
[24]

Montero-Camacho, Y

P. Montero-Camacho, Y. Zhang and Y. Mao,The long-lasting effect of X-ray pre-heating in the post-reionization intergalactic medium,Mon. Not. R. Astron. Soc.529(2024) 3666 [2307.10598]

work page arXiv 2024
[25]

Greig and A

B. Greig and A. Mesinger,Simultaneously constraining the astrophysics of reionisation and the epoch of heating with 21CMMC, inPeering towards Cosmic Dawn, V. Jeli´ c and T. van der Hulst, eds., vol. 333 ofIAU Symposium, pp. 18–21, May, 2018, DOI [1705.03471]

work page arXiv 2018
[26]

Murray, B

S. Murray, B. Greig, A. Mesinger, J. Mu˜ noz, Y. Qin, J. Park et al.,21cmFAST v3: A Python-integrated C code for generating 3D realizations of the cosmic 21cm signal.,The Journal of Open Source Software5(2020) 2582 [2010.15121]

work page arXiv 2020
[27]

Cranmer, A

M. Cranmer, A. Sanchez-Gonzalez, P. Battaglia, R. Xu, K. Cranmer, D. Spergel et al., Discovering Symbolic Models from Deep Learning with Inductive Biases,arXiv e-prints(2020) arXiv:2006.11287 [2006.11287]

work page arXiv 2020
[28]

Interpretable Machine Learning for Science with PySR and SymbolicRegression.jl

M. Cranmer,Interpretable Machine Learning for Science with PySR and SymbolicRegression.jl,arXiv e-prints(2023) arXiv:2305.01582 [2305.01582]

work page internal anchor Pith review arXiv 2023
[29]

Aghanim et al

Planck Collaboration, N. Aghanim, Y. Akrami, M. Ashdown, J. Aumont, C. Baccigalupi et al.,Planck 2018 results. V. CMB power spectra and likelihoods,Astron. Astrophys.641 (2020) A5 [1907.12875]

work page arXiv 2018
[30]

Delouis, L

J.M. Delouis, L. Pagano, S. Mottet, J.L. Puget and L. Vibert,SRoll2: an improved mapmaking approach to reduce large-scale systematic effects in the Planck High Frequency Instrument legacy maps,Astron. Astrophys.629(2019) A38 [1901.11386]

work page arXiv 2019
[31]

Akrami, K

Planck Collaboration, Y. Akrami, K.J. Andersen, M. Ashdown, C. Baccigalupi, M. Ballardini et al.,Planck intermediate results. LVII. Joint Planck LFI and HFI data processing,Astron. Astrophys.643(2020) A42 [2007.04997]

work page arXiv 2020
[32]

Efstathiou and S

G. Efstathiou and S. Gratton,A Detailed Description of the CamSpec Likelihood Pipeline and a Reanalysis of the Planck High Frequency Maps,arXiv e-prints(2019) arXiv:1910.00483 [1910.00483]

work page arXiv 2019
[33]

Rosenberg, S

E. Rosenberg, S. Gratton and G. Efstathiou,CMB power spectra and cosmological parameters from Planck PR4 with CamSpec,Mon. Not. R. Astron. Soc.517(2022) 4620 [2205.10869]

work page arXiv 2022
[34]

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

T. Louis, A. La Posta, Z. Atkins, H.T. Jense, I. Abril-Cabezas, G.E. Addison et al.,The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods andΛCDM Parameters, arXiv e-prints(2025) arXiv:2503.14452 [2503.14452]

work page internal anchor Pith review arXiv 2025
[35]

Hirata and U

C.M. Hirata and U. Seljak,Reconstruction of lensing from the cosmic microwave background polarization,Phys. Rev. D68(2003) 083002 [astro-ph/0306354]

work page arXiv 2003
[36]

F.J. Qu, B.D. Sherwin, M.S. Madhavacheril, D. Han, K.T. Crowley, I. Abril-Cabezas et al., The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and Its Implications for Structure Growth,Astrophys. J.962(2024) 112 [2304.05202]

work page arXiv 2024
[37]

Madhavacheril, F.J

M.S. Madhavacheril, F.J. Qu, B.D. Sherwin, N. MacCrann, Y. Li, I. Abril-Cabezas et al.,The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters,Astrophys. J.962(2024) 113 [2304.05203]. – 28 –

work page arXiv 2024
[38]

MacCrann, B.D

N. MacCrann, B.D. Sherwin, F.J. Qu, T. Namikawa, M.S. Madhavacheril, I. Abril-Cabezas et al.,The Atacama Cosmology Telescope: Mitigating the impact of extragalactic foregrounds for the DR6 CMB lensing analysis,arXiv e-prints(2023) arXiv:2304.05196 [2304.05196]

work page arXiv 2023
[39]

Farren, A

G.S. Farren, A. Krolewski, N. MacCrann, S. Ferraro, I. Abril-Cabezas, R. An et al.,The Atacama Cosmology Telescope: Cosmology from cross-correlations of unWISE galaxies and ACT DR6 CMB lensing,arXiv e-prints(2023) arXiv:2309.05659 [2309.05659]

work page arXiv 2023
[40]

Carron, M

J. Carron, M. Mirmelstein and A. Lewis,CMB lensing from Planck PR4 maps,J. Cosmol. Astropart. Phys.2022(2022) 039 [2206.07773]

work page arXiv 2022
[41]

Aghanim et al

Planck Collaboration, N. Aghanim, Y. Akrami, M. Ashdown, J. Aumont, C. Baccigalupi et al.,Planck 2018 results. VIII. Gravitational lensing,Astron. Astrophys.641(2020) A8 [1807.06210]

work page arXiv 2018
[42]

Giar` e, E

W. Giar` e, E. Di Valentino and A. Melchiorri,Measuring the reionization optical depth without large-scale CMB polarization,arXiv e-prints(2023) arXiv:2312.06482 [2312.06482]

work page arXiv 2023
[43]

J. Wang, Z. Huang, Y. Yao, J. Liu, L. Huang and Y. Su,A PAge-like Unified Dark Fluid model,J. Cosmol. Astropart. Phys.2024(2024) 053 [2405.05798]

work page arXiv 2024
[44]

C. Zhao, S. Huang, M. He, P. Montero-Camacho, Y. Liu, P. Renard et al.,MUltiplexed Survey Telescope: Perspectives for Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Survey,arXiv e-prints(2024) arXiv:2411.07970 [2411.07970]

work page internal anchor Pith review Pith/arXiv arXiv 2024
[45]

DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations

A.G. Adame, J. Aguilar, S. Ahlen, S. Alam, D.M. Alexander, M. Alvarez et al.,DESI 2024 VI: cosmological constraints from the measurements of baryon acoustic oscillations,J. Cosmol. Astropart. Phys.2025(2025) 021 [2404.03002]

work page internal anchor Pith review arXiv 2024
[46]

DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints

DESI Collaboration, M. Abdul Karim, J. Aguilar, S. Ahlen, S. Alam, L. Allen et al.,DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints, arXiv e-prints(2025) arXiv:2503.14738 [2503.14738]

work page internal anchor Pith review arXiv 2025
[47]

F. Qin, Y. Wang and G.-B. Zhao,J-PAS and PFS surveys in the era of dark energy and neutrino mass measurements,arXiv e-prints(2025) arXiv:2505.04275 [2505.04275]

work page arXiv 2025
[48]

Abareshi, J

DESI Collaboration, B. Abareshi, J. Aguilar, S. Ahlen, S. Alam, D.M. Alexander et al., Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument,Astron. J. 164(2022) 207 [2205.10939]

work page arXiv 2022
[49]

Abdul Karim et al

DESI Collaboration, M. Abdul-Karim, J. Aguilar, S. Ahlen, C. Allende Prieto, O. Alves et al.,DESI DR2 Results I: Baryon Acoustic Oscillations from the Lyman Alpha Forest,arXiv e-prints(2025) arXiv:2503.14739 [2503.14739]

work page arXiv 2025
[50]

The Dark Energy Sur- vey: Cosmology Results with ∼1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set,

DES Collaboration, T.M.C. Abbott, M. Acevedo, M. Aguena, A. Alarcon, S. Allam et al., The Dark Energy Survey: Cosmology Results with∼1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set,Astrophys. J. Lett.973(2024) L14 [2401.02929]

work page arXiv 2024
[51]

The Pantheon+ Analysis: The Full Dataset and Light-Curve Release

D. Scolnic, D. Brout, A. Carr, A.G. Riess, T.M. Davis, A. Dwomoh et al.,The Pantheon+ Analysis: The Full Data Set and Light-curve Release,Astrophys. J.938(2022) 113 [2112.03863]

work page internal anchor Pith review arXiv 2022
[52]

The Pantheon+ Analysis: Cosmological Constraints

D. Brout, D. Scolnic, B. Popovic, A.G. Riess, A. Carr, J. Zuntz et al.,The Pantheon+ Analysis: Cosmological Constraints,Astrophys. J.938(2022) 110 [2202.04077]

work page internal anchor Pith review arXiv 2022
[53]

Rubin et al.,Union Through UNITY: Cosmology with 2,000 SNe Using a Unified Bayesian Framework,Astrophys

D. Rubin, G. Aldering, M. Betoule, A. Fruchter, X. Huang, A.G. Kim et al.,Union Through UNITY: Cosmology with 2,000 SNe Using a Unified Bayesian Framework,arXiv e-prints (2023) arXiv:2311.12098 [2311.12098]

work page arXiv 2023
[54]

D. Blas, J. Lesgourgues and T. Tram,The Cosmic Linear Anisotropy Solving System (CLASS). Part II: Approximation schemes,J. Cosmol. Astropart. Phys.2011(2011) 034 [1104.2933]. – 29 –

work page internal anchor Pith review arXiv 2011
[55]

Greig, A

B. Greig, A. Mesinger, F.B. Davies, F. Wang, J. Yang and J.F. Hennawi,IGM damping wing constraints on reionization from covariance reconstruction of two z≳7 QSOs,Mon. Not. R. Astron. Soc.512(2022) 5390 [2112.04091]

work page arXiv 2022
[56]

Greig et al.,IGM damping wing constraints on the tail end of reionization from the enlarged XQR-30 sample,Mon

B. Greig, A. Mesinger, E. Ba˜ nados, G.D. Becker, S.E.I. Bosman, H. Chen et al.,IGM damping wing constraints on the tail end of reionization from the enlarged XQR-30 sample, Mon. Not. R. Astron. Soc.530(2024) 3208 [2404.12585]

work page arXiv 2024
[57]

Spina, S.E.I

B. Spina, S.E.I. Bosman, F.B. Davies, P. Gaikwad and Y. Zhu,Damping wings in the Lyman-αforest: A model-independent measurement of the neutral fraction at 5.4 ¡ z ¡ 6.1, Astron. Astrophys.688(2024) L26 [2405.12273]

work page arXiv 2024
[58]

ˇDurovˇ c´ ıkov´ a, A.-C

D. ˇDurovˇ c´ ıkov´ a, A.-C. Eilers, H. Chen, S. Satyavolu, G. Kulkarni, R.A. Simcoe et al., Chronicling the Reionization History at 6≲z≲7 with Emergent Quasar Damping Wings, Astrophys. J.969(2024) 162 [2401.10328]

work page arXiv 2024
[59]

Huberty, C

M. Huberty, C. Scarlata, M.J. Hayes and S. Gazagnes,The Pitfalls of Using Lyman Alpha Damping Wings in High-z Galaxy Spectra to Measure the Intergalactic Neutral Hydrogen Fraction,arXiv e-prints(2025) arXiv:2501.13899 [2501.13899]

work page arXiv 2025
[60]

Bruton, C

S. Bruton, C. Scarlata, F. Haardt, M.J. Hayes, C. Mason, A.M. Morales et al.,The Impact of Cosmic Variance on Inferences of Global Neutral Fraction Derived from LyαLuminosity Functions during Reionization,Astrophys. J.953(2023) 29 [2305.04949]

work page arXiv 2023
[61]

McGreer, A

I.D. McGreer, A. Mesinger and V. D’Odorico,Model-independent evidence in favour of an end to reionization by z≈6,Mon. Not. R. Astron. Soc.447(2015) 499 [1411.5375]

work page arXiv 2015
[62]

Elbers,Rapid late-time reionization: constraints and cosmological implications,arXiv e-prints(2025) arXiv:2508.21069 [2508.21069]

W. Elbers,Rapid late-time reionization: constraints and cosmological implications,arXiv e-prints(2025) arXiv:2508.21069 [2508.21069]

work page arXiv 2025
[63]

Y. Qin, A. Mesinger, D. Prelogovi´ c, G. Becker, M. Bischetti, S. Bosman et al.,Percent-level timing of reionisation: Self-consistent, implicit-likelihood inference from XQR-30+ Lyαforest data,Publ. Astron. Soc. Aust.42(2025) e049 [2412.00799]

work page arXiv 2025
[64]

Cobaya: Code for Bayesian Analysis of hierarchical physical models

J. Torrado and A. Lewis,Cobaya: code for Bayesian analysis of hierarchical physical models, J. Cosmol. Astropart. Phys.2021(2021) 057 [2005.05290]

work page internal anchor Pith review arXiv 2021
[65]

Cosmological parameters from CMB and other data: a Monte-Carlo approach

A. Lewis and S. Bridle,Cosmological parameters from CMB and other data: A Monte Carlo approach,Phys. Rev. D66(2002) 103511 [astro-ph/0205436]

work page Pith review arXiv 2002
[66]

Efficient sampling of fast and slow cosmological parameters

A. Lewis,Efficient sampling of fast and slow cosmological parameters,Phys. Rev. D87(2013) 103529 [1304.4473]

work page Pith review arXiv 2013
[67]

Gelman and D.B

A. Gelman and D.B. Rubin,Inference from Iterative Simulation Using Multiple Sequences, Statistical Science7(1992) 457

1992
[68]

Y. Li, J.R. Eimer, J.W. Appel, C.L. Bennett, M.K. Brewer, S.M. Bruno et al.,A Measurement of the Largest-scale CMB E-mode Polarization with CLASS,Astrophys. J.986 (2025) 111 [2501.11904]

work page arXiv 2025
[69]

Paoletti, D.K

D. Paoletti, D.K. Hazra, F. Finelli and G.F. Smoot,Extended reionization in models beyond ΛCDM with Planck 2018 data,J. Cosmol. Astropart. Phys.2020(2020) 005 [2005.12222]

work page arXiv 2018
[70]

Abdurashidova, J.E

Z. Abdurashidova, J.E. Aguirre, P. Alexander, Z.S. Ali, Y. Balfour, R. Barkana et al.,HERA Phase I Limits on the Cosmic 21 cm Signal: Constraints on Astrophysics and Cosmology during the Epoch of Reionization,Astrophys. J.924(2022) 51 [2108.07282]

work page arXiv 2022
[72]

Munshi, F.G

S. Munshi, F.G. Mertens, J.K. Chege, L.V.E. Koopmans, A.R. Offringa, B. Semelin et al., – 30 – Improved upper limits on the 21-cm signal power spectrum atz= 17.0andz= 20.3from an optimal field observed with NenuFAR,arXiv e-prints(2025) arXiv:2507.10533 [2507.10533]

work page arXiv 2025
[73]

Fragoset al., X-ray Binary Evolution Across Cos- mic Time, Astrophys

T. Fragos, B. Lehmer, M. Tremmel, P. Tzanavaris, A. Basu-Zych, K. Belczynski et al.,X-Ray Binary Evolution Across Cosmic Time,Astrophys. J.764(2013) 41 [1206.2395]

work page arXiv 2013
[74]

Mineo, M

S. Mineo, M. Gilfanov and R. Sunyaev,X-ray emission from star-forming galaxies - I. High-mass X-ray binaries,Mon. Not. R. Astron. Soc.419(2012) 2095 [1105.4610]

work page arXiv 2012
[75]

MNRAS491(2), 1736–1745 (2020) https://doi.org/10.1093/ mnras/stz3083 arXiv:1905.12640 [astro-ph.CO]

L.C. Keating, L.H. Weinberger, G. Kulkarni, M.G. Haehnelt, J. Chardin and D. Aubert,Long troughs in the Lyman-αforest below redshift 6 due to islands of neutral hydrogen,Mon. Not. R. Astron. Soc.491(2020) 1736 [1905.12640]

work page arXiv 2020
[76]

Nasir and A

F. Nasir and A. D’Aloisio,Observing the tail of reionization: neutral islands in the z = 5.5 Lyman-αforest,Mon. Not. R. Astron. Soc.494(2020) 3080 [1910.03570]

work page arXiv 2020
[77]

C. Cain, A. D’Aloisio, N. Gangolli and G.D. Becker,A Short Mean Free Path at z = 6 Favors Late and Rapid Reionization by Faint Galaxies,Astrophys. J. Lett.917(2021) L37 [2105.10511]

work page arXiv 2021
[78]

Zhu, G.D

Y. Zhu, G.D. Becker, S.E.I. Bosman, L.C. Keating, V. D’Odorico, R.L. Davies et al.,Long Dark Gaps in the LyβForest at z ¡ 6: Evidence of Ultra-late Reionization from XQR-30 Spectra,Astrophys. J.932(2022) 76 [2205.04569]

work page arXiv 2022
[79]

Bosman, F.B

S.E.I. Bosman, F.B. Davies, G.D. Becker, L.C. Keating, R.L. Davies, Y. Zhu et al.,Hydrogen reionization ends by z = 5.3: Lyman-αoptical depth measured by the XQR-30 sample,Mon. Not. R. Astron. Soc.514(2022) 55 [2108.03699]

work page arXiv 2022
[80]

Gao, J.X

A. Gao, J.X. Prochaska, Z. Cai, S. Zou, C. Zhao, Z. Sun et al.,Measuring the Mean Free Path of H I Ionizing Photons at 3.2≤z≤4.6 with DESI Y1 Quasars,Astrophys. J. Lett.981 (2025) L27 [2411.15838]

work page arXiv 2025
[81]

Morales, C.A

A.M. Morales, C.A. Mason, S. Bruton, M. Gronke, F. Haardt and C. Scarlata,The Evolution of the Lyman-alpha Luminosity Function during Reionization,Astrophys. J.919(2021) 120 [2101.01205]

work page arXiv 2021

Showing first 80 references.