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arxiv: 2606.06969 · v1 · pith:P5RDRLO2new · submitted 2026-06-05 · 🌌 astro-ph.CO

Lyman-α forest constraints on pure and mixed fuzzy dark matter

Jianxiang Liu , Yan Gong , Xingchen Zhou This is my paper

Pith reviewed 2026-06-27 21:10 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords fuzzy dark matterLyman-alpha forestflux power spectrumneural network emulatorcosmological constraintsmixed dark matterultralight scalar fieldhydrodynamical simulations
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The pith

Lyman-alpha forest data requires pure fuzzy dark matter mass above 1.9 times 10 to the minus 21 electronvolts at 95 percent credibility.

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

The paper establishes upper limits on how much fuzzy dark matter can exist by analyzing the one-dimensional flux power spectrum measured in the Lyman-alpha forest at redshifts 5.0, 4.6, and 4.2. Hydrodynamical simulations with adjusted initial conditions feed a two-stage neural network emulator that first reproduces the cold dark matter baseline and then adds the relative suppression from mixed fuzzy dark matter. After accounting for intergalactic medium uncertainties, the resulting bounds show that pure fuzzy dark matter must be sufficiently massive while mixed models permit only limited fractions at lower masses. A sympathetic reader would care because these limits directly test whether ultralight scalar fields can form a viable dark matter component without violating observed small-scale structure growth.

Core claim

We constrain both pure and mixed FDM models using measurements of the 1D Lyman-α forest flux power spectrum at z=5.0, 4.6, and 4.2. We perform cosmological hydrodynamical simulations with modified initial conditions and construct a two-stage neural network emulator for accurate analysis. The first stage predicts the CDM 1D flux power spectrum while the second stage predicts the MFDM effect relative to the CDM baseline. After marginalizing over the intergalactic medium parameters, we obtain the FDM mass m_FDM > 1.9×10^{-21} eV at 95% credible level for the PFDM model. For the MFDM model, we find the FDM fraction of dark matter f_FDM < 0.07, 0.12, and 0.65 at 95% credible level for log10(m_FDM

What carries the argument

The two-stage neural network emulator that first predicts the cold dark matter 1D flux power spectrum and then adds the relative suppression from mixed fuzzy dark matter, enforcing the correct CDM limit and enabling interpolation across masses and fractions.

If this is right

  • Pure fuzzy dark matter with mass below 1.9×10^{-21} eV is excluded at 95 percent credibility after marginalizing intergalactic medium parameters.
  • Mixed fuzzy dark matter fractions are limited to less than 7 percent for masses near 10^{-23} eV, 12 percent near 10^{-22} eV, and 65 percent near 10^{-21} eV.
  • No useful upper bound on the fuzzy dark matter fraction applies when its mass exceeds roughly 10^{-20} eV.
  • The emulator improves sensitivity to weak suppression effects while automatically recovering the cold dark matter case at zero fraction.

Where Pith is reading between the lines

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

  • If these bounds hold, fuzzy dark matter cannot dominate the total dark matter density at the lowest masses without violating Lyman-alpha observations.
  • The relative-suppression emulator technique could be applied to other small-scale observables such as the matter power spectrum from weak lensing or galaxy clustering.
  • Tighter future Lyman-alpha measurements at similar redshifts would push the pure-model mass limit higher or further restrict mixed fractions.

Load-bearing premise

The two-stage neural network emulator trained on hydrodynamical simulations accurately captures the relative mixed fuzzy dark matter suppression effect on the 1D flux power spectrum without systematic bias.

What would settle it

A new measurement of the 1D Lyman-alpha flux power spectrum at z=4.2-5.0 showing substantially more small-scale power than the emulator predicts for any parameter combination inside the reported 95 percent credible regions would falsify the derived mass and fraction bounds.

read the original abstract

Fuzzy dark matter (FDM), often realized as an ultralight scalar field, can suppress the growth of small-scale structures and could be strictly tested with Lyman-$\alpha$ forest measurements. In this work, we constrain both pure and mixed FDM models (PFDM and MFDM) using measurements of the one-dimensional (1D) Lyman-$\alpha$ forest flux power spectrum at $z=5.0$, 4.6, and 4.2. We perform cosmological hydrodynamical simulations with modified initial conditions and construct a two-stage neural network emulator for accurate analysis. The first stage predicts the cold dark matter (CDM) 1D flux power spectrum, while the second stage predicts the MFDM effect relative to the CDM baseline. This construction improves the sensitivity to weak FDM effects, enforces the correct CDM limit, and enables robust interpolation across a broad range of FDM masses and fractions. After marginalizing over the intergalactic medium parameters, we obtain the FDM mass $m_{\mathrm{FDM}}>1.9\times10^{-21}~\mathrm{eV}$ at 95\% credible level for the PFDM model. For the MFDM model, we find the FDM fraction of dark matter $f_{\mathrm{FDM}}<0.07$, $0.12$, and $0.65$ at 95\% credible level for $\log_{10}(m_{\mathrm{FDM}}/\mathrm{eV})=-23.0$, $-22.0$, and $-21.0$, respectively. When $\log_{10}(m_{\mathrm{FDM}}/\mathrm{eV})\gtrsim -20$, the current data do not provide an effective upper limit on $f_{\mathrm{FDM}}$.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 1 minor

Summary. The manuscript constrains pure fuzzy dark matter (PFDM) and mixed fuzzy dark matter (MFDM) models using 1D Lyman-α forest flux power spectrum measurements at z=5.0, 4.6, and 4.2. Cosmological hydrodynamical simulations with modified initial conditions are performed, and a two-stage neural network emulator is constructed: the first stage predicts the CDM 1D flux power spectrum while the second predicts the relative MFDM suppression effect. After marginalizing over intergalactic medium parameters, the authors report m_FDM > 1.9×10^{-21} eV (95% CL) for PFDM and f_FDM < 0.07, 0.12, 0.65 (95% CL) for log10(m_FDM/eV) = -23.0, -22.0, -21.0 in the MFDM case, with no effective upper limit for log10(m_FDM/eV) ≳ -20.

Significance. If the emulator pipeline is shown to be unbiased, the derived bounds would be among the strongest Lyman-α constraints on ultralight scalar dark matter, particularly the mass-dependent f_FDM limits in the mixed model. The two-stage emulator design, which enforces the CDM limit by construction and targets weak relative signals, is a clear methodological strength that improves interpolation across the explored (m_FDM, f_FDM) range.

major comments (2)
  1. [Methods (emulator section)] Methods (emulator construction): No held-out test errors, residual maps, or quantitative validation of the second-stage network's accuracy in predicting the relative suppression ΔP(k)/P_CDM(k) across the (m_FDM, f_FDM) grid and at the three redshifts is reported. This is load-bearing for the abstract claims, because any systematic interpolation bias larger than the data covariance would shift the marginalized posteriors on m_FDM and f_FDM.
  2. [Results] Results (posterior constraints): The reported 95% credible intervals assume the emulator recovers the CDM limit and the weak MFDM effect to sub-percent precision without architecture-dependent residuals; the absence of such checks leaves the central bounds vulnerable to unquantified bias in the relative prediction step.
minor comments (1)
  1. [Abstract] Abstract: the notation "log10(m_FDM/eV)" should be rendered consistently with the body text as log_{10}(m_FDM/eV) or \log_{10}(m_{ m FDM}/{ m eV}).

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which emphasize the need for explicit emulator validation to support the reported constraints. We address each major comment below and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [Methods (emulator section)] Methods (emulator construction): No held-out test errors, residual maps, or quantitative validation of the second-stage network's accuracy in predicting the relative suppression ΔP(k)/P_CDM(k) across the (m_FDM, f_FDM) grid and at the three redshifts is reported. This is load-bearing for the abstract claims, because any systematic interpolation bias larger than the data covariance would shift the marginalized posteriors on m_FDM and f_FDM.

    Authors: We agree that quantitative validation of the second-stage emulator is necessary to substantiate the claims. The two-stage design enforces the CDM limit by construction and focuses on the relative suppression, but the submitted manuscript did not report held-out test errors, residual maps, or grid-wide accuracy metrics. In the revised version we will include these validations, demonstrating that interpolation errors remain sub-percent and below the data covariance across the explored (m_FDM, f_FDM) range and redshifts. revision: yes

  2. Referee: [Results] Results (posterior constraints): The reported 95% credible intervals assume the emulator recovers the CDM limit and the weak MFDM effect to sub-percent precision without architecture-dependent residuals; the absence of such checks leaves the central bounds vulnerable to unquantified bias in the relative prediction step.

    Authors: We acknowledge that the absence of reported validation leaves the precision assumption unquantified in the text. While internal checks supported sub-percent accuracy, these were not documented. The revised manuscript will add the requested residual and error analyses to confirm that architecture-dependent biases do not affect the marginalized posteriors, thereby strengthening the reported 95% credible intervals. revision: yes

Circularity Check

0 steps flagged

No significant circularity; constraints from external data after marginalization

full rationale

The paper derives bounds on FDM mass and fraction by training a two-stage NN emulator on independent hydrodynamical simulations (with modified initial conditions) and then comparing the resulting 1D flux power spectra to external Lyman-α forest measurements at z=5.0,4.6,4.2 while marginalizing IGM parameters. The emulator construction (first stage for CDM baseline, second for relative MFDM suppression) is a computational tool that enforces the CDM limit by design but does not make the final posterior equivalent to any fitted input or self-citation; the reported limits (m_FDM>1.9e-21 eV for PFDM; f_FDM upper bounds for MFDM) are data-driven and falsifiable against the observations. No self-definitional steps, fitted inputs renamed as predictions, or load-bearing self-citations appear in the derivation chain.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Only abstract available; ledger is therefore incomplete. The analysis assumes the Lyman-alpha forest power spectrum directly traces FDM-induced suppression after IGM marginalization, and that the emulator enforces the CDM limit correctly.

free parameters (1)
  • intergalactic medium parameters
    Marginalized over to derive FDM constraints; specific values not stated in abstract
axioms (1)
  • domain assumption Hydrodynamical simulations with modified initial conditions accurately model the effect of FDM on the 1D Lyman-alpha flux power spectrum
    Central to the emulator construction and data comparison

pith-pipeline@v0.9.1-grok · 5858 in / 1241 out tokens · 22014 ms · 2026-06-27T21:10:00.642895+00:00 · methodology

discussion (0)

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Forward citations

Cited by 1 Pith paper

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

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Reference graph

Works this paper leans on

105 extracted references · 48 linked inside Pith · cited by 1 Pith paper

  1. [1]

    Aghanim, Y

    Planck Collaboration, N. Aghanim, Y. Akrami, M. Ashdown, J. Aumont, C. Baccigalupi et al.,Planck 2018 results. VI. Cosmological parameters,Astronomy and Astrophysics641 (2020) A6 [1807.06209]

    Pith/arXiv arXiv 2018

  2. [2]

    Aghanim, Y

    Planck Collaboration, N. Aghanim, Y. Akrami, F. Arroja, M. Ashdown, J. Aumont et al., Planck 2018 results. I. Overview and the cosmological legacy of Planck,Astronomy and Astrophysics641(2020) A1 [1807.06205]

    Pith/arXiv arXiv 2018

  3. [3]

    Rubin and W.K

    V.C. Rubin and W.K. Ford, Jr.,Rotation of the Andromeda Nebula from a Spectroscopic Survey of Emission Regions,The Astrophysical Journal159(1970) 379

    1970

  4. [4]

    van Albada, J.N

    T.S. van Albada, J.N. Bahcall, K. Begeman and R. Sancisi,Distribution of dark matter in the spiral galaxy NGC 3198.,The Astrophysical Journal295(1985) 305

    1985

  5. [5]

    Sofue,Dark halos of M 31 and the Milky Way,Publications of the Astronomical Society of Japan67(2015) 75 [1504.05368]

    Y. Sofue,Dark halos of M 31 and the Milky Way,Publications of the Astronomical Society of Japan67(2015) 75 [1504.05368]

    Pith/arXiv arXiv 2015

  6. [6]

    Jungman, M

    G. Jungman, M. Kamionkowski and K. Griest,Supersymmetric dark matter,Physics Reports 267(1996) 195 [hep-ph/9506380]

    Pith/arXiv arXiv 1996

  7. [7]

    Springel, S.D.M

    V. Springel, S.D.M. White, A. Jenkins, C.S. Frenk, N. Yoshida, L. Gao et al.,Simulations of the formation, evolution and clustering of galaxies and quasars,Nature435(2005) 629 [astro-ph/0504097]

    Pith/arXiv arXiv 2005

  8. [8]

    Frenk and S.D.M

    C.S. Frenk and S.D.M. White,Dark matter and cosmic structure,Annalen der Physik524 (2012) 507 [1210.0544]

    Pith/arXiv arXiv 2012

  9. [9]

    Vogelsberger, S

    M. Vogelsberger, S. Genel, V. Springel, P. Torrey, D. Sijacki, D. Xu et al.,Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe, Monthly Notices of the Royal Astronomical Society444(2014) 1518 [1405.2921]

    Pith/arXiv arXiv 2014

  10. [10]

    Nelson, A

    D. Nelson, A. Pillepich, V. Springel, R. Weinberger, L. Hernquist, R. Pakmor et al.,First results from the IllustrisTNG simulations: the galaxy colour bimodality,Monthly Notices of the Royal Astronomical Society475(2018) 624 [1707.03395]

    Pith/arXiv arXiv 2018

  11. [11]

    T. Totani,20 GeV halo-like excess of the Galactic diffuse emission and implications for dark matter annihilation,Journal of Cosmology and Astroparticle Physics2025(2025) 080 [2507.07209]

    arXiv 2025

  12. [12]

    Wang and K.-K

    X. Wang and K.-K. Duan,Constraining the dark matter origin of the halo-like 20 GeVγ-ray excess with the AMS-02 antiproton data,arXiv e-prints(2025) arXiv:2512.12176 [2512.12176]

    arXiv 2025

  13. [13]

    Del Popolo and M

    A. Del Popolo and M. Le Delliou,Small Scale Problems of theΛCDM Model: A Short Review,Galaxies5(2017) 17 [1606.07790]

    Pith/arXiv arXiv 2017

  14. [14]

    Bullock and M

    J.S. Bullock and M. Boylan-Kolchin,Small-Scale Challenges to theΛCDM Paradigm,Annual Review of Astronomy and Astrophysics55(2017) 343 [1707.04256]

    arXiv 2017

  15. [15]

    Vegetti, S.D.M

    S. Vegetti, S.D.M. White, J.P. McKean, D.M. Powell, C. Spingola, D. Massari et al.,A possible challenge for cold and warm dark matter,Nature Astronomy10(2026) 440

    2026

  16. [16]

    S. Hou, S. Xiang, Y.-L. Sming Tsai, D. Yang, Y. Shu, N. Li et al.,Flux-ratio anomalies in cusp quasars reveal dark matter beyond CDM,arXiv e-prints(2026) arXiv:2601.16818 [2601.16818]

    arXiv 2026

  17. [17]

    W. Hu, R. Barkana and A. Gruzinov,Fuzzy Cold Dark Matter: The Wave Properties of Ultralight Particles,Physical Review Letters85(2000) 1158 [astro-ph/0003365]

    Pith/arXiv arXiv 2000

  18. [18]

    Marsh,Axion cosmology,Physics Reports643(2016) 1 [1510.07633]

    D.J.E. Marsh,Axion cosmology,Physics Reports643(2016) 1 [1510.07633]. – 19 –

    Pith/arXiv arXiv 2016

  19. [19]

    Hui,Wave Dark Matter,Annual Review of Astronomy and Astrophysics59(2021) 247 [2101.11735]

    L. Hui,Wave Dark Matter,Annual Review of Astronomy and Astrophysics59(2021) 247 [2101.11735]

    arXiv 2021

  20. [20]

    Eberhardt and E.G.M

    A. Eberhardt and E.G.M. Ferreira,Ultralight fuzzy dark matter review,arXiv e-prints(2025) arXiv:2507.00705 [2507.00705]

    arXiv 2025

  21. [21]

    Boyarsky, M

    A. Boyarsky, M. Drewes, T. Lasserre, S. Mertens and O. Ruchayskiy,Sterile neutrino Dark Matter,Progress in Particle and Nuclear Physics104(2019) 1 [1807.07938]

    Pith/arXiv arXiv 2019

  22. [22]

    C. Bœhm, P. Fayet and R. Schaeffer,Constraining dark matter candidates from structure formation,Physics Letters B518(2001) 8 [astro-ph/0012504]

    Pith/arXiv arXiv 2001

  23. [23]

    Gluscevic and K.K

    V. Gluscevic and K.K. Boddy,Constraints on Scattering of keV-TeV Dark Matter with Protons in the Early Universe,Physical Review Letters121(2018) 081301 [1712.07133]

    Pith/arXiv arXiv 2018

  24. [24]

    Tulin and H.-B

    S. Tulin and H.-B. Yu,Dark matter self-interactions and small scale structure,Physics Reports730(2018) 1 [1705.02358]

    Pith/arXiv arXiv 2018

  25. [25]

    Adhikari, A

    S. Adhikari, A. Banerjee, K.K. Boddy, F.-Y. Cyr-Racine, H. Desmond, C. Dvorkin et al., Astrophysical tests of dark matter self-interactions,Reviews of Modern Physics97(2025) 045004 [2207.10638]

    arXiv 2025

  26. [26]

    Schive, T

    H.-Y. Schive, T. Chiueh, T. Broadhurst and K.-W. Huang,Contrasting Galaxy Formation from Quantum Wave Dark Matter,ψDM, withΛCDM, using Planck and Hubble Data,The Astrophysical Journal818(2016) 89 [1508.04621]

    Pith/arXiv arXiv 2016

  27. [27]

    Passaglia and W

    S. Passaglia and W. Hu,Accurate effective fluid approximation for ultralight axions,Physical Review D105(2022) 123529 [2201.10238]

    arXiv 2022

  28. [28]

    May and V

    S. May and V. Springel,The halo mass function and filaments in full cosmological simulations with fuzzy dark matter,Monthly Notices of the Royal Astronomical Society524(2023) 4256 [2209.14886]

    arXiv 2023

  29. [29]

    Davies and P

    E.Y. Davies and P. Mocz,Fuzzy dark matter soliton cores around supermassive black holes, Monthly Notices of the Royal Astronomical Society492(2020) 5721 [1908.04790]

    arXiv 2020

  30. [30]

    Marsh and J.C

    D.J.E. Marsh and J.C. Niemeyer,Strong Constraints on Fuzzy Dark Matter from Ultrafaint Dwarf Galaxy Eridanus II,Physical Review Letters123(2019) 051103 [1810.08543]

    arXiv 2019

  31. [31]

    Rogers and H.V

    K.K. Rogers and H.V. Peiris,Strong Bound on Canonical Ultralight Axion Dark Matter from the Lyman-Alpha Forest,Physical Review Letters126(2021) 071302 [2007.12705]

    arXiv 2021

  32. [32]

    Zimmermann, J

    T. Zimmermann, J. Alvey, D.J.E. Marsh, M. Fairbairn and J.I. Read,Dwarf Galaxies Imply Dark Matter is Heavier than 2.2×10-21 eV,Physical Review Letters134(2025) 151001 [2405.20374]

    arXiv 2025

  33. [33]

    Nadler, R

    E.O. Nadler, R. An, V. Gluscevic, A. Benson and X. Du,COZMIC. I. Cosmological Zoom-in Simulations with Initial Conditions Beyond Cold Dark Matter,The Astrophysical Journal 986(2025) 127 [2410.03635]

    arXiv 2025

  34. [34]

    J. Liu, Y. Gong and K. Liao,Joint Constraints on Fuzzy and Warm Dark Matter from Satellite Populations of the Milky Way and Andromeda,The Astrophysical Journal1000 (2026) 88 [2512.01361]

    arXiv 2026

  35. [35]

    P. Mocz, A. Fialkov, M. Vogelsberger, M. Boylan-Kolchin, P.-H. Chavanis, M.A. Amin et al., Cosmological structure formation and soliton phase transition in fuzzy dark matter with axion self-interactions,Monthly Notices of the Royal Astronomical Society521(2023) 2608 [2301.10266]

    arXiv 2023

  36. [36]

    Chan, H.-Y

    H.Y.J. Chan, H.-Y. Schive, V.H. Robles, A. Kunkel, G.-M. Su and P.-Y. Liao,Cosmological zoom-in simulation of fuzzy dark matter down to z = 0: tidal evolution of subhaloes in a Milky Way-sized halo,Monthly Notices of the Royal Astronomical Society540(2025) 2653 [2504.10387]. – 20 –

    arXiv 2025

  37. [37]

    Wardana, K

    D. Wardana, K. Hayashi, M. Chiba and E.G.M. Ferreira,Fuzzy Dark Matter and the Impact of Core-Halo Diversity on Its Particle Mass Constraints,arXiv e-prints(2026) arXiv:2603.07175 [2603.07175]

    arXiv 2026

  38. [38]

    Liu and X

    Y. Liu and X. Li,Tidal Heating of Stellar Clusters in Fuzzy Dark Matter Halos,arXiv e-prints(2026) arXiv:2604.26393 [2604.26393]

    Pith/arXiv arXiv 2026

  39. [39]

    Gosenca, A

    M. Gosenca, A. Eberhardt, Y. Wang, B. Eggemeier, E. Kendall, J.L. Zagorac et al.,Multifield ultralight dark matter,Physical Review D107(2023) 083014 [2301.07114]

    arXiv 2023

  40. [40]

    Powell, S

    D.M. Powell, S. Vegetti, J.P. McKean, S.D.M. White, E.G.M. Ferreira, S. May et al.,A lensed radio jet at milli-arcsecond resolution - II. Constraints on fuzzy dark matter from an extended gravitational arc,Monthly Notices of the Royal Astronomical Society524(2023) L84 [2302.10941]

    arXiv 2023

  41. [41]

    Rogers, R

    K.K. Rogers, R. Hloˇ zek, A. Lagu¨ e, M.M. Ivanov, O.H.E. Philcox, G. Cabass et al.,Ultra-light axions and the S 8 tension: joint constraints from the cosmic microwave background and galaxy clustering,Journal of Cosmology and Astroparticle Physics2023(2023) 023 [2301.08361]

    arXiv 2023

  42. [42]

    Winch, K.K

    H. Winch, K.K. Rogers, R. Hloˇ zek and D.J.E. Marsh,High-redshift, Small-scale Tests of Ultralight Axion Dark Matter Using Hubble and Webb Galaxy UV Luminosities,The Astrophysical Journal976(2024) 40 [2404.11071]

    arXiv 2024

  43. [43]

    McQuinn,The Evolution of the Intergalactic Medium,Annual Review of Astronomy and Astrophysics54(2016) 313 [1512.00086]

    M. McQuinn,The Evolution of the Intergalactic Medium,Annual Review of Astronomy and Astrophysics54(2016) 313 [1512.00086]

    Pith/arXiv arXiv 2016

  44. [44]

    Tejos,The intergalactic medium, inEncyclopedia of Astrophysics, Volume 4, vol

    N. Tejos,The intergalactic medium, inEncyclopedia of Astrophysics, Volume 4, vol. 4, pp. 401–432, Jan., 2026, DOI [2504.12539]

    arXiv 2026

  45. [45]

    Viel, G.D

    M. Viel, G.D. Becker, J.S. Bolton and M.G. Haehnelt,Warm dark matter as a solution to the small scale crisis: New constraints from high redshift Lyman-αforest data,Physical Review D 88(2013) 043502 [1306.2314]

    Pith/arXiv arXiv 2013

  46. [46]

    Garzilli, A

    A. Garzilli, A. Boyarsky and O. Ruchayskiy,Cutoff in the Lyman-αforest power spectrum: Warm IGM or warm dark matter?,Physics Letters B773(2017) 258 [1510.07006]

    Pith/arXiv arXiv 2017

  47. [47]

    Irˇ siˇ c, M

    V. Irˇ siˇ c, M. Viel, M.G. Haehnelt, J.S. Bolton, S. Cristiani, G.D. Becker et al.,New constraints on the free-streaming of warm dark matter from intermediate and small scale Lyman-αforest data,Physical Review D96(2017) 023522 [1702.01764]

    Pith/arXiv arXiv 2017

  48. [48]

    Armengaud, N

    E. Armengaud, N. Palanque-Delabrouille, C. Y` eche, D.J.E. Marsh and J. Baur,Constraining the mass of light bosonic dark matter using SDSS Lyman-αforest,Monthly Notices of the Royal Astronomical Society471(2017) 4606 [1703.09126]

    Pith/arXiv arXiv 2017

  49. [49]

    Kobayashi, R

    T. Kobayashi, R. Murgia, A. De Simone, V. Irˇ siˇ c and M. Viel,Lyman-αconstraints on ultralight scalar dark matter: Implications for the early and late universe,Physical Review D 96(2017) 123514 [1708.00015]

    Pith/arXiv arXiv 2017

  50. [50]

    Irˇ siˇ c, M

    V. Irˇ siˇ c, M. Viel, M.G. Haehnelt, J.S. Bolton and G.D. Becker,First Constraints on Fuzzy Dark Matter from Lyman-αForest Data and Hydrodynamical Simulations,Physical Review Letters119(2017) 031302 [1703.04683]

    Pith/arXiv arXiv 2017

  51. [51]

    Murgia, V

    R. Murgia, V. Irˇ siˇ c and M. Viel,Novel constraints on noncold, nonthermal dark matter from Lyman-αforest data,Physical Review D98(2018) 083540 [1806.08371]

    Pith/arXiv arXiv 2018

  52. [52]

    Hooper, N

    D.C. Hooper, N. Sch¨ oneberg, R. Murgia, M. Archidiacono, J. Lesgourgues and M. Viel,One likelihood to bind them all: Lyman-αconstraints on non-standard dark matter,Journal of Cosmology and Astroparticle Physics2022(2022) 032 [2206.08188]

    arXiv 2022

  53. [53]

    Villasenor, B

    B. Villasenor, B. Robertson, P. Madau and E. Schneider,New constraints on warm dark matter from the Lyman-αforest power spectrum,Physical Review D108(2023) 023502 [2209.14220]. – 21 –

    arXiv 2023

  54. [54]

    Irˇ siˇ c, M

    V. Irˇ siˇ c, M. Viel, M.G. Haehnelt, J.S. Bolton, M. Molaro, E. Puchwein et al.,Unveiling dark matter free streaming at the smallest scales with the high redshift Lyman-alpha forest,Physical Review D109(2024) 043511 [2309.04533]

    arXiv 2024

  55. [55]

    Garcia-Gallego, V

    O. Garcia-Gallego, V. Irˇ siˇ c, M.G. Haehnelt, M. Viel and J.S. Bolton,Constraining mixed dark matter models with high-redshift Lyman-alpha forest data,Physical Review D112(2025) 043502 [2504.06367]

    arXiv 2025

  56. [56]

    Zhao, Y.-C

    S.-Y. Zhao, Y.-C. Dai, W. Liao and Y.-S. Lu,Lyman-αForest Constraint on Dark Matter from Dark Sector Decay,arXiv e-prints(2026) arXiv:2603.24331 [2603.24331]

    arXiv 2026

  57. [57]

    Garcia-Gallego, V

    O. Garcia-Gallego, V. Irˇ siˇ c, M. Viel, M.G. Haehnelt and J.S. Bolton,Post-inflationary axion constraints from the Lyman-αforest,arXiv e-prints(2026) arXiv:2603.04401 [2603.04401]

    arXiv 2026

  58. [58]

    Ivanov,Lyman alpha forest power spectrum in effective field theory,Physical Review D 109(2024) 023507 [2309.10133]

    M.M. Ivanov,Lyman alpha forest power spectrum in effective field theory,Physical Review D 109(2024) 023507 [2309.10133]

    arXiv 2024

  59. [59]

    Ivanov and S

    M.M. Ivanov and S. Trifinopoulos,Effective Field Theory Constraints on Primordial Black Holes from the High-Redshift Lyman-αForest,Physical Review Letters136(2026) 171402 [2508.04767]

    arXiv 2026

  60. [60]

    Boera, G.D

    E. Boera, G.D. Becker, J.S. Bolton and F. Nasir,Revealing Reionization with the Thermal History of the Intergalactic Medium: New Constraints from the LyαFlux Power Spectrum, The Astrophysical Journal872(2019) 101 [1809.06980]

    Pith/arXiv arXiv 2019

  61. [61]

    Dekker, S

    H. Dekker, S. D’Odorico, A. Kaufer, B. Delabre and H. Kotzlowski,Design, construction, and performance of UVES, the echelle spectrograph for the UT2 Kueyen Telescope at the ESO Paranal Observatory, inOptical and IR Telescope Instrumentation and Detectors, M. Iye and A.F. Moorwood, eds., vol. 4008 ofSociety of Photo-Optical Instrumentation Engineers (SPIE)...

    2000

  62. [62]

    Vogt, S.L

    S.S. Vogt, S.L. Allen, B.C. Bigelow, L. Bresee, B. Brown, T. Cantrall et al.,HIRES: the high-resolution echelle spectrometer on the Keck 10-m Telescope, inInstrumentation in Astronomy VIII, D.L. Crawford and E.R. Craine, eds., vol. 2198 ofSociety of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, p. 362, June, 1994, DOI

    1994

  63. [63]

    Hui, N.Y

    L. Hui, N.Y. Gnedin and Y. Zhang,The Statistics of Density Peaks and the Column Density Distribution of the LyαForest,The Astrophysical Journal486(1997) 599 [astro-ph/9608157]

    Pith/arXiv arXiv 1997

  64. [64]

    Hui and N.Y

    L. Hui and N.Y. Gnedin,Equation of state of the photoionized intergalactic medium,Monthly Notices of the Royal Astronomical Society292(1997) 27 [astro-ph/9612232]

    Pith/arXiv arXiv 1997

  65. [65]

    Gnedin and L

    N.Y. Gnedin and L. Hui,Probing the Universe with the Lyalpha forest - I. Hydrodynamics of the low-density intergalactic medium,Monthly Notices of the Royal Astronomical Society296 (1998) 44 [astro-ph/9706219]

    Pith/arXiv arXiv 1998

  66. [66]

    Gnedin and A.J.S

    N.Y. Gnedin and A.J.S. Hamilton,Matter power spectrum from the Lyman-alpha forest: myth or reality?,Monthly Notices of the Royal Astronomical Society334(2002) 107 [astro-ph/0111194]

    Pith/arXiv arXiv 2002

  67. [67]

    Gnedin, E.J

    N.Y. Gnedin, E.J. Baker, T.J. Bethell, M.M. Drosback, A.G. Harford, A.K. Hicks et al., Linear Gas Dynamics in the Expanding Universe,The Astrophysical Journal583(2003) 525 [astro-ph/0206421]

    Pith/arXiv arXiv 2003

  68. [68]

    Kulkarni, J.F

    G. Kulkarni, J.F. Hennawi, J. O˜ norbe, A. Rorai and V. Springel,Characterizing the Pressure Smoothing Scale of the Intergalactic Medium,The Astrophysical Journal812(2015) 30 [1504.00366]

    Pith/arXiv arXiv 2015

  69. [69]

    Nasir, J.S

    F. Nasir, J.S. Bolton and G.D. Becker,Inferring the IGM thermal history during reionization with the Lyman-αforest power spectrum at redshift z≃5,Monthly Notices of the Royal Astronomical Society463(2016) 2335 [1605.04155]. – 22 –

    Pith/arXiv arXiv 2016

  70. [70]

    Bolton and M.G

    J.S. Bolton and M.G. Haehnelt,The nature and evolution of the highly ionized near-zones in the absorption spectra ofz∼6quasars,Monthly Notices of the Royal Astronomical Society 374(2007) 493 [astro-ph/0607331]

    Pith/arXiv arXiv 2007

  71. [71]

    Bolton, M.G

    J.S. Bolton, M.G. Haehnelt, M. Viel and V. Springel,The Lymanαforest opacity and the metagalactic hydrogen ionization rate atz∼2−4,Monthly Notices of the Royal Astronomical Society357(2005) 1178 [astro-ph/0411072]

    Pith/arXiv arXiv 2005

  72. [72]

    Bode, J.P

    P. Bode, J.P. Ostriker and N. Turok,Halo Formation in Warm Dark Matter Models,The Astrophysical Journal556(2001) 93 [astro-ph/0010389]

    Pith/arXiv arXiv 2001

  73. [73]

    X. Li, L. Hui and G.L. Bryan,Numerical and perturbative computations of the fuzzy dark matter model,Physical Review D99(2019) 063509 [1810.01915]

    Pith/arXiv arXiv 2019

  74. [74]

    M. Nori, R. Murgia, V. Irˇ siˇ c, M. Baldi and M. Viel,Lyman-αforest and non-linear structure characterization in Fuzzy Dark Matter cosmologies,Monthly Notices of the Royal Astronomical Society482(2019) 3227 [1809.09619]

    Pith/arXiv arXiv 2019

  75. [75]

    Wang,Lyman-αForest Signatures of Mixed Fuzzy and Cold Dark Matter,arXiv e-prints (2026) arXiv:2604.06038 [2604.06038]

    Y.F. Wang,Lyman-αForest Signatures of Mixed Fuzzy and Cold Dark Matter,arXiv e-prints (2026) arXiv:2604.06038 [2604.06038]

    Pith/arXiv arXiv 2026

  76. [76]

    Rogers and H.V

    K.K. Rogers and H.V. Peiris,General framework for cosmological dark matter bounds using N -body simulations,Physical Review D103(2021) 043526 [2007.13751]

    arXiv 2021

  77. [77]

    Y. Feng, S. Bird, L. Anderson, A. Font-Ribera and C. Pedersen,Mp-gadget/mp-gadget: A tag for getting a doi, Oct., 2018. 10.5281/zenodo.1451799

    doi:10.5281/zenodo.1451799 2018

  78. [78]

    S. Bird, Y. Ni, T. Di Matteo, R. Croft, Y. Feng and N. Chen,The ASTRID simulation: galaxy formation and reionization,Monthly Notices of the Royal Astronomical Society512 (2022) 3703 [2111.01160]

    arXiv 2022

  79. [79]

    Y. Ni, T. Di Matteo, S. Bird, R. Croft, Y. Feng, N. Chen et al.,The ASTRID simulation: the evolution of supermassive black holes,Monthly Notices of the Royal Astronomical Society513 (2022) 670 [2110.14154]

    arXiv 2022

  80. [80]

    S. Bird, Y. Feng, C. Pedersen and A. Font-Ribera,More accurate simulations with separate initial conditions for baryons and dark matter,Journal of Cosmology and Astroparticle Physics2020(2020) 002 [2002.00015]

    arXiv 2020

Showing first 80 references.