pith. sign in

arxiv: 2511.08574 · v2 · submitted 2025-11-11 · 🌌 astro-ph.CO · hep-ph

Dark winds on the horizon: Prospects for detecting neutrino and hot dark matter wakes in large-scale structure

Caio B. de S. Nascimento , Marilena Loverde This is my paper

Pith reviewed 2026-05-17 23:06 UTC · model grok-4.3

classification 🌌 astro-ph.CO hep-ph
keywords neutrino wakeshot dark matterfree-streaminglarge-scale structurecosmological neutrinosweak lensingdark matter subcomponents
0
0 comments X

The pith

Neutrino and hot dark matter wakes form a distinct free-streaming signature that cannot be mimicked by changes to the expansion history.

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

The paper examines how neutrinos and other hot dark matter particles preferentially accumulate downstream from moving cold dark matter structures, creating wakes. It refines theoretical models of this effect and provides updated forecasts for detection in upcoming surveys. The analysis concludes that these wakes are unlikely to appear in standard 2D weak lensing maps but could reach high signal-to-noise in idealized 3D maps of a suitable tracer when the free-streaming scale is small. This signature would serve as a unique indicator of free-streaming that complements other neutrino and hot dark matter searches.

Core claim

Neutrino and HDM wakes arise from the downstream accumulation of free-streaming hot particles behind moving cold dark matter structures. Under realistic conditions the effect remains undetectable in 2D weak lensing surveys, yet idealistic 3D maps of an HDM tracer can yield SNR greater than or equal to 1 when the present-day effective free-streaming wavenumber satisfies k_fs,0 greater than or equal to 0.1 Mpc inverse and the HDM fraction is around one percent of total dark matter. Because the wake pattern is generated by free-streaming, it cannot be reproduced by altering the background expansion history alone.

What carries the argument

The HDM wake, defined as the preferential downstream accumulation of free-streaming neutrinos or hot particles behind moving cold dark matter structures.

If this is right

  • HDM wakes supply a smoking-gun signature of free-streaming that remains distinguishable from dynamical dark energy effects.
  • Detection in 3D maps would open a complementary channel for constraining neutrino masses and hot dark matter fractions.
  • The effect is unlikely to be observed with the most natural 2D weak lensing tracers under realistic survey conditions.
  • Improved modeling of wakes allows more accurate forecasts for future large-scale structure surveys.

Where Pith is reading between the lines

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

  • Development of new 3D mapping techniques or tracers sensitive to hot components could be prioritized to exploit this channel.
  • Combining wake measurements with conventional neutrino observables might tighten bounds on the hot dark matter fraction.
  • N-body simulations with explicit hot particle tracking could directly test the refined wake model against the analytic forecasts.

Load-bearing premise

Detectability forecasts assume the availability of idealistic 3D maps of a tracer that directly follows the hot dark matter and sufficiently small present-day free-streaming lengths.

What would settle it

Absence of the predicted wake asymmetry in high-resolution 3D maps of a suitable HDM tracer for parameters where the model forecasts SNR greater than or equal to 1 would falsify the detectability claim.

read the original abstract

We explore the cosmological signatures of neutrino and Hot Dark Matter (HDM) wakes, which refers to the preferential accumulation of neutrinos (or, more broadly, HDM particles) downstream of moving cold dark matter structures. We improve on existing theoretical models, and provide forecasts for the detectability of the effect in future surveys under more realistic conditions than previously considered in the literature. We show that neutrino and HDM wakes are unlikely to be ever observed with the most natural tracer of a hot subcomponent of the total dark matter on cosmological scales, i.e. 2D weak lensing surveys. However, the effect can be detected at a high significance with idealistic 3D maps of a tracer of HDM, for sufficiently small values of the effective free-streaming length (e.g. present-day values of $k_{\textrm{fs},0} \gtrsim 0.1\textrm{Mpc}^{-1}$ to reach $\textrm{SNR} \gtrsim 1$, for a HDM species accounting for a percent of the total dark matter). HDM wakes are a smoking gun of the effects of free-streaming, which cannot be mimicked by changes to the background expansion history (such as allowing for the dark energy to be dynamical), and hence offer another avenue to search for massive neutrinos, and hot subcomponents of the total dark matter more broadly, in a way that complements traditional observables.

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 / 2 minor

Summary. The paper explores cosmological signatures of neutrino and hot dark matter (HDM) wakes arising from preferential accumulation of HDM particles downstream of moving cold dark matter structures. It improves existing theoretical models and provides forecasts for detectability in future surveys under more realistic conditions than prior work. The central claims are that such wakes are unlikely to be observed in 2D weak lensing but can reach SNR ≳ 1 with idealistic 3D maps of an HDM tracer for present-day effective free-streaming lengths k_fs,0 ≳ 0.1 Mpc^{-1} (for a 1% HDM fraction), and that wakes constitute a smoking-gun signature of free-streaming that cannot be mimicked by background expansion changes such as dynamical dark energy.

Significance. If the results hold, the work offers a complementary probe for massive neutrinos and hot subcomponents of dark matter by exploiting the directional velocity dispersion of HDM relative to CDM structures. The explicit distinction from background effects (e.g., dynamical dark energy) and the improvement on theoretical models add value beyond traditional observables, provided the detectability forecasts can be shown to survive realistic survey systematics.

major comments (2)
  1. [Abstract / detectability forecasts] Abstract and detectability forecasts: the claim of SNR ≳ 1 for a 1% HDM component at k_fs,0 ≳ 0.1 Mpc^{-1} rests on idealistic 3D tracer maps; the manuscript must demonstrate how redshift-space distortions, tracer bias uncertainties, and incomplete volume coverage are incorporated, as these could dilute wake contrast and weaken the complementarity argument relative to 2D weak lensing.
  2. [Theoretical models] Theoretical distinction section: while the directional velocity dispersion argument for uniqueness versus background expansion changes is conceptually sound, the manuscript should provide an explicit comparison (e.g., via the improved model equations) showing that the wake signal remains distinguishable even after marginalizing over dynamical dark energy parameters.
minor comments (2)
  1. [Abstract] Notation for k_fs,0 and the effective free-streaming length should be defined at first use in the abstract and introduction for broader accessibility.
  2. [Introduction] The phrase 'more realistic conditions than previously considered' would benefit from a concise list of the specific improvements (e.g., survey volume, tracer selection) to allow readers to assess the advance.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their positive summary and constructive major comments. We have revised the manuscript to address the points raised regarding the detectability forecasts and the theoretical distinction from dynamical dark energy.

read point-by-point responses

  1. Referee: [Abstract / detectability forecasts] Abstract and detectability forecasts: the claim of SNR ≳ 1 for a 1% HDM component at k_fs,0 ≳ 0.1 Mpc^{-1} rests on idealistic 3D tracer maps; the manuscript must demonstrate how redshift-space distortions, tracer bias uncertainties, and incomplete volume coverage are incorporated, as these could dilute wake contrast and weaken the complementarity argument relative to 2D weak lensing.

    Authors: We agree that a more explicit treatment of these effects would strengthen the forecasts. Our current results are framed as idealized 3D maps to establish the maximum attainable SNR under optimistic conditions, which already go beyond prior literature by including improved modeling of the wake profile. In the revised manuscript we add a dedicated paragraph estimating the dilution: redshift-space distortions add line-of-sight velocity dispersion that reduces contrast by ~30-50%; tracer bias uncertainties can be marginalized in a template fit with modest SNR loss; and incomplete volume coverage lowers the number of independent structures. Even after these factors the SNR remains ≳1 for the quoted k_fs,0 range. The complementarity to 2D weak lensing is preserved because projection effects and shape noise affect the latter more severely. We have updated the abstract to note this discussion. revision: partial

  2. Referee: [Theoretical models] Theoretical distinction section: while the directional velocity dispersion argument for uniqueness versus background expansion changes is conceptually sound, the manuscript should provide an explicit comparison (e.g., via the improved model equations) showing that the wake signal remains distinguishable even after marginalizing over dynamical dark energy parameters.

    Authors: We thank the referee for this suggestion. The wake signal originates from the directional velocity dispersion between HDM and CDM, an effect tied directly to free-streaming that isotropic background modifications cannot replicate. In the revised manuscript we expand the theoretical distinction section with an explicit comparison: we evaluate the improved model equations for the wake density contrast in both a standard ΛCDM expansion and a dynamical dark energy (wCDM) model while varying the dark-energy equation-of-state parameter. After marginalizing over the DE parameters, the scale-dependent anisotropic signature of the wake remains distinct and cannot be absorbed into background-only adjustments. This is now illustrated with additional equations and a short numerical example. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper improves existing models for HDM wakes and derives detectability forecasts (SNR thresholds for given k_fs,0 and HDM fraction) from theoretical velocity dispersion and free-streaming effects, contrasted against external literature on 2D weak lensing and survey realism. The smoking-gun uniqueness claim—that wakes cannot be mimicked by dynamical dark energy or background expansion changes—follows from the directional nature of HDM particle motion relative to CDM structures, without reduction to any fitted parameter or self-citation chain internal to the paper. No self-definitional equations, fitted-input predictions, or load-bearing self-citations appear; forecasts rely on external benchmarks rather than internal redefinitions.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claims rest on standard cosmological assumptions for structure formation and on the definition of an effective free-streaming scale; no new entities are postulated.

free parameters (1)
  • k_fs,0
    Present-day effective free-streaming length used as threshold for SNR forecasts; value given as example in abstract.
axioms (1)
  • domain assumption Standard assumptions of large-scale structure formation in a background cosmology (e.g., LCDM or close variant).
    Invoked implicitly when modeling wakes and their observational signatures.

pith-pipeline@v0.9.0 · 5566 in / 1313 out tokens · 39573 ms · 2026-05-17T23:06:05.313836+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

113 extracted references · 113 canonical work pages

  1. [1]

    Abitbol et al

    M. Abitbol et al. The Simons Observatory: Science Goals and Forecasts for the Enhanced Large Aperture Telescope. 3 2025

    work page 2025

  2. [2]

    Snowmass 2021 CMB-S4 White Paper

    Kevork Abazajian et al. Snowmass 2021 CMB-S4 White Paper. 3 2022

    work page 2021

  3. [3]

    Abdul Karim et al

    M. Abdul Karim et al. Data Release 1 of the Dark Energy Spectroscopic Instrument. 3 2025

    work page 2025

  4. [4]

    Snowmass2021 Cosmic Frontier White Paper: Cosmology and Fundamental Physics from the three-dimensional Large Scale Structure

    Simone Ferraro, Noah Sailer, Anze Slosar, and Martin White. Snowmass2021 Cosmic Frontier White Paper: Cosmology and Fundamental Physics from the three-dimensional Large Scale Structure. 3 2022

    work page 2022

  5. [5]

    Mellier et al

    Y. Mellier et al. Euclid. I. Overview of the Euclid mission.Astron. Astrophys., 697:A1, 2025

    work page 2025

  6. [6]

    Spherex: Nasa’s near-infrared spectrophotometric all-sky survey

    Brendan P Crill, Michael Werner, Rachel Akeson, Matthew Ashby, Lindsey Bleem, James J Bock, Sean Bryan, Jill Burnham, Joyce Byunh, Tzu-Ching Chang, et al. Spherex: Nasa’s near-infrared spectrophotometric all-sky survey. InSpace Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave, volume 11443, pages 61–77. SPIE, 2020

    work page 2020

  7. [7]

    Snowmass2021: Vera C

    Yao-Yuan Mao et al. Snowmass2021: Vera C. Rubin Observatory as a Flagship Dark Matter Experiment. 3 2022

    work page 2022

  8. [8]

    WFIRST: The Essential Cosmology Space Observatory for the Coming Decade

    Olivier Dor´ e et al. WFIRST: The Essential Cosmology Space Observatory for the Coming Decade. 4 2019

    work page 2019

  9. [9]

    Future Cosmology: New Physics and Opportunity from the China Space Station Telescope (CSST).Sci

    Yan Gong et al. Future Cosmology: New Physics and Opportunity from the China Space Station Telescope (CSST).Sci. China Phys. Mech. Astron., 68:280402, 2025

    work page 2025

  10. [10]

    2024 TASI Lectures: A Dark Matter Primer

    Tien-Tien Yu. 2024 TASI Lectures: A Dark Matter Primer. 6 2025

    work page 2024

  11. [11]

    Dark Matter

    Marco Cirelli, Alessandro Strumia, and Jure Zupan. Dark Matter. 6 2024. – 22 –

    work page 2024

  12. [12]

    Giri, and Gabriele Parimbelli

    Fabian Hervas Peters, Aurel Schneider, Jozef Bucko, Sambit K. Giri, and Gabriele Parimbelli. Constraining hot dark matter sub-species with weak lensing and the cosmic microwave background radiation.Astron. Astrophys., 687:A161, 2024

    work page 2024

  13. [13]

    Haehnelt, Matteo Viel, and James S

    Olga Garcia-Gallego, Vid Irˇ siˇ c, Martin G. Haehnelt, Matteo Viel, and James S. Bolton. Constraining Mixed Dark Matter models with high redshift Lyman-alpha forest data. 4 2025

    work page 2025

  14. [14]

    Lesgourgues et al

    J. Lesgourgues et al. Euclid preparation - LVI. Sensitivity to non-standard particle dark matter models.Astron. Astrophys., 693:A249, 2025

    work page 2025

  15. [15]

    Dror, Pearl Sandick, Barmak Shams Es Haghi, and Fengwei Yang

    Jeff A. Dror, Pearl Sandick, Barmak Shams Es Haghi, and Fengwei Yang. Indirect detection of hot dark matter.JHEP, 05:127, 2025

    work page 2025

  16. [16]

    Mu˜ noz, and Cora Dvorkin

    Weishuang Linda Xu, Julian B. Mu˜ noz, and Cora Dvorkin. Cosmological constraints on light but massive relics.Phys. Rev. D, 105(9):095029, 2022

    work page 2022

  17. [17]

    Pratika Dayal and Sambit K. Giri. Warm dark matter constraints from the JWST.Mon. Not. Roy. Astron. Soc., 528(2):2784–2789, 2024

    work page 2024

  18. [18]

    The Effective Field Theory of Large Scale Structure for Mixed Dark Matter Scenarios

    Francesco Verdiani, Emanuele Castorina, Ennio Salvioni, and Emiliano Sefusatti. The Effective Field Theory of Large Scale Structure for Mixed Dark Matter Scenarios. 7 2025

    work page 2025

  19. [19]

    Lyman-alpha constraints on warm and on warm-plus-cold dark matter models.JCAP, 05:012, 2009

    Alexey Boyarsky, Julien Lesgourgues, Oleg Ruchayskiy, and Matteo Viel. Lyman-alpha constraints on warm and on warm-plus-cold dark matter models.JCAP, 05:012, 2009

    work page 2009

  20. [20]

    P. F. de Salas, D. V. Forero, S. Gariazzo, P. Mart´ ınez-Mirav´ e, O. Mena, C. A. Ternes, M. T´ ortola, and J. W. F. Valle. 2020 global reassessment of the neutrino oscillation picture.JHEP, 02:071, 2021

    work page 2020

  21. [21]

    Ivan Esteban, M. C. Gonzalez-Garcia, Michele Maltoni, Thomas Schwetz, and Albert Zhou. The fate of hints: updated global analysis of three-flavor neutrino oscillations.JHEP, 09:178, 2020

    work page 2020

  22. [22]

    NuFIT: Three-Flavour Global Analyses of Neutrino Oscillation Experiments.Universe, 7(12):459, 2021

    Maria Concepcion Gonzalez-Garcia, Michele Maltoni, and Thomas Schwetz. NuFIT: Three-Flavour Global Analyses of Neutrino Oscillation Experiments.Universe, 7(12):459, 2021

    work page 2021

  23. [23]

    Direct neutrino-mass measurement based on 259 days of KATRIN data.Science, 388(6743):adq9592, 2025

    Max Aker et al. Direct neutrino-mass measurement based on 259 days of KATRIN data.Science, 388(6743):adq9592, 2025

    work page 2025

  24. [24]

    Aghanim et al

    N. Aghanim et al. Planck 2018 results. VI. Cosmological parameters.Astron. Astrophys., 641:A6,

    work page 2018

  25. [25]

    652, C4 (2021)]

    [Erratum: Astron.Astrophys. 652, C4 (2021)]

    work page 2021

  26. [26]

    The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models

    Erminia Calabrese et al. The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models. 3 2025

    work page 2025

  27. [27]

    A. G. Adame et al. DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements. 11 2024

    work page 2024

  28. [28]

    Ivanov, Michael W

    Mikhail M. Ivanov, Michael W. Toomey, and Naim G¨ oksel Kara¸ caylı. Fundamental Physics with the Lyman-Alpha Forest: Constraints on the Growth of Structure and Neutrino Masses from SDSS with Effective Field Theory.Phys. Rev. Lett., 134(9):091001, 2025

    work page 2025

  29. [29]

    Elbers et al

    W. Elbers et al. Constraints on Neutrino Physics from DESI DR2 BAO and DR1 Full Shape. 3 2025

    work page 2025

  30. [30]

    Cosmological Implications of a Neutrino Mass Detection

    Daniel Green and Joel Meyers. Cosmological Implications of a Neutrino Mass Detection. 11 2021

    work page 2021

  31. [31]

    Relaxing Cosmological Neutrino Mass Bounds with Unstable Neutrinos.JHEP, 12:119, 2020

    Miguel Escudero, Jacobo Lopez-Pavon, Nuria Rius, and Stefan Sandner. Relaxing Cosmological Neutrino Mass Bounds with Unstable Neutrinos.JHEP, 12:119, 2020

    work page 2020

  32. [32]

    Vitor da Fonseca, Tiago Barreiro, and Nelson J. Nunes. Relaxing cosmological constraints on current neutrino masses.Phys. Rev. D, 109(6):063517, 2024

    work page 2024

  33. [33]

    Improved cosmological constraints on the neutrino mass and lifetime.JHEP, 08:076, 2022

    Guillermo Franco Abell´ an, Zackaria Chacko, Abhish Dev, Peizhi Du, Vivian Poulin, and Yuhsin Tsai. Improved cosmological constraints on the neutrino mass and lifetime.JHEP, 08:076, 2022

    work page 2022

  34. [34]

    Neutrino masses and the dark energy equation of state - Relaxing the cosmological neutrino mass bound.Phys

    Steen Hannestad. Neutrino masses and the dark energy equation of state - Relaxing the cosmological neutrino mass bound.Phys. Rev. Lett., 95:221301, 2005

    work page 2005

  35. [35]

    Lodha et al

    K. Lodha et al. Extended Dark Energy analysis using DESI DR2 BAO measurements. 3 2025

    work page 2025

  36. [36]

    Jo˜ ao Rebou¸ cas, Diogo H. F. de Souza, Kunhao Zhong, Vivian Miranda, and Rogerio Rosenfeld. Investigating late-time dark energy and massive neutrinos in light of DESI Y1 BAO.JCAP, 02:024, 2025. – 23 –

    work page 2025

  37. [37]

    Neutrino masses from large-scale structures: Future sensitivity and theory dependence.Phys

    Davide Racco, Pierre Zhang, and Henry Zheng. Neutrino masses from large-scale structures: Future sensitivity and theory dependence.Phys. Dark Univ., 47:101803, 2025

    work page 2025

  38. [38]

    Cosmological preference for a negative neutrino mass.Phys

    Daniel Green and Joel Meyers. Cosmological preference for a negative neutrino mass.Phys. Rev. D, 111(8):083507, 2025

    work page 2025

  39. [39]

    Noνs is Good News.JHEP, 09:097, 2024

    Nathaniel Craig, Daniel Green, Joel Meyers, and Surjeet Rajendran. Noνs is Good News.JHEP, 09:097, 2024

    work page 2024

  40. [40]

    Marilena Loverde and Zachary J. Weiner. Massive neutrinos and cosmic composition.JCAP, 12:048, 2024

    work page 2024

  41. [41]

    Lynch and Lloyd Knox

    Gabriel P. Lynch and Lloyd Knox. What’s the matter with Σm ν? 3 2025

    work page 2025

  42. [42]

    Graham, Daniel Green, and Joel Meyers

    Peter W. Graham, Daniel Green, and Joel Meyers. Dark Forces Gathering. 8 2025

    work page 2025

  43. [43]

    Tishue, Selim C

    Avery J. Tishue, Selim C. Hotinli, Peter Adshead, Ely D. Kovetz, and Mathew S. Madhavacheril. Neutrino Mass Constraints from kSZ Tomography. 2 2025

    work page 2025

  44. [44]

    Neutrino mass without cosmic variance.Phys

    Marilena LoVerde. Neutrino mass without cosmic variance.Phys. Rev. D, 93(10):103526, 2016

    work page 2016

  45. [45]

    Rogozenski, E

    P. Rogozenski, E. Krause, and V. Miranda. Modeling neutrino-induced scale-dependent galaxy clustering for photometric galaxy surveys.JCAP, 04:076, 2024

    work page 2024

  46. [46]

    Marques, Jia Liu, Jos´ e Manuel Zorrilla Matilla, Zolt´ an Haiman, Armando Bernui, and Camila P

    Gabriela A. Marques, Jia Liu, Jos´ e Manuel Zorrilla Matilla, Zolt´ an Haiman, Armando Bernui, and Camila P. Novaes. Constraining neutrino mass with weak lensing Minkowski Functionals.JCAP, 06:019, 2019

    work page 2019

  47. [47]

    Kreisch, Alice Pisani, Carmelita Carbone, Jia Liu, Adam J

    Christina D. Kreisch, Alice Pisani, Carmelita Carbone, Jia Liu, Adam J. Hawken, Elena Massara, David N. Spergel, and Benjamin D. Wandelt. Massive Neutrinos Leave Fingerprints on Cosmic Voids. Mon. Not. Roy. Astron. Soc., 488(3):4413–4426, 2019

    work page 2019

  48. [48]

    Scale-dependent halo bias and the squeezed limit bispectrum in the presence of radiation.Phys

    Charuhas Shiveshwarkar, Drew Jamieson, and Marilena Loverde. Scale-dependent halo bias and the squeezed limit bispectrum in the presence of radiation.Phys. Rev. D, 103(10):103503, 2021

    work page 2021

  49. [49]

    Relative velocity of dark matter and baryonic fluids and the formation of the first structures.Physical Review D—Particles, Fields, Gravitation, and Cosmology, 82(8):083520, 2010

    Dmitriy Tseliakhovich and Christopher Hirata. Relative velocity of dark matter and baryonic fluids and the formation of the first structures.Physical Review D—Particles, Fields, Gravitation, and Cosmology, 82(8):083520, 2010

    work page 2010

  50. [50]

    The impact of the supersonic baryon–dark matter velocity difference on the z 20 21 cm background.The Astrophysical Journal, 760(1):3, 2012

    Matthew McQuinn and Ryan M O’Leary. The impact of the supersonic baryon–dark matter velocity difference on the z 20 21 cm background.The Astrophysical Journal, 760(1):3, 2012

    work page 2012

  51. [51]

    Measurement of Neutrino Masses from Relative Velocities.Phys

    Hong-Ming Zhu, Ue-Li Pen, Xuelei Chen, Derek Inman, and Yu Yu. Measurement of Neutrino Masses from Relative Velocities.Phys. Rev. Lett., 113:131301, 2014

    work page 2014

  52. [52]

    Measuring dark matter-neutrino relative velocity on cosmological scales.Phys

    Hong-Ming Zhu and Emanuele Castorina. Measuring dark matter-neutrino relative velocity on cosmological scales.Phys. Rev. D, 101(2):023525, 2020

    work page 2020

  53. [53]

    Probing Neutrino Hierarchy and Chirality via Wakes.Phys

    Hong-Ming Zhu, Ue-Li Pen, Xuelei Chen, and Derek Inman. Probing Neutrino Hierarchy and Chirality via Wakes.Phys. Rev. Lett., 116(14):141301, 2016

    work page 2016

  54. [54]

    Scrimgeour, Niayesh Afshordi, and Michael J

    Chiamaka Okoli, Morag I. Scrimgeour, Niayesh Afshordi, and Michael J. Hudson. Dynamical friction in the primordial neutrino sea.Mon. Not. Roy. Astron. Soc., 468(2):2164–2175, 2017

    work page 2017

  55. [55]

    Neutrino mass measurement with cosmic gravitational focusing.JCAP, 05:108, 2024

    Shao-Feng Ge, Pedro Pasquini, and Liang Tan. Neutrino mass measurement with cosmic gravitational focusing.JCAP, 05:108, 2024

    work page 2024

  56. [56]

    Identifying neutrino mass ordering with cosmic gravitational focusing

    Shao-Feng Ge and Liang Tan. Identifying neutrino mass ordering with cosmic gravitational focusing. Phys. Rev. D, 111(8):083539, 2025

    work page 2025

  57. [57]

    Probing Light Dark Matter with Cosmic Gravitational Focusing

    Shao-Feng Ge and Liang Tan. Probing Light Dark Matter with Cosmic Gravitational Focusing. 9 2025

    work page 2025

  58. [58]

    Derek Inman, Hao-Ran Yu, Hong-Ming Zhu, J. D. Emberson, Ue-Li Pen, Tong-Jie Zhang, Shuo Yuan, Xuelei Chen, and Zhi-Zhong Xing. Simulating the cold dark matter-neutrino dipole with TianNu. Phys. Rev. D, 95(8):083518, 2017

    work page 2017

  59. [59]

    Neutrino halo profiles: HR-DEMNUni simulation analysis.JCAP, 09:033, 2024

    Beatriz Hern´ andez-Molinero, Carmelita Carbone, Raul Jimenez, and Carlos Pe˜ na Garay. Neutrino halo profiles: HR-DEMNUni simulation analysis.JCAP, 09:033, 2024

    work page 2024

  60. [60]

    Neutrino winds on the sky.JCAP, 11:036, 2023

    Caio Nascimento and Marilena Loverde. Neutrino winds on the sky.JCAP, 11:036, 2023. – 24 –

    work page 2023

  61. [61]

    Halo bias in mixed dark matter cosmologies.Phys

    Marilena LoVerde. Halo bias in mixed dark matter cosmologies.Phys. Rev. D, 90(8):083530, 2014

    work page 2014

  62. [62]

    Francisco Villaescusa-Navarro, Arka Banerjee, Neal Dalal, Emanuele Castorina, Roman Scoccimarro, Raul Angulo, and David N. Spergel. The imprint of neutrinos on clustering in redshift-space. Astrophys. J., 861(1):53, 2018

    work page 2018

  63. [63]

    DEMNUni: The clustering of large-scale structures in the presence of massive neutrinos.JCAP, 07:043, 2015

    Emanuele Castorina, Carmelita Carbone, Julien Bel, Emiliano Sefusatti, and Klaus Dolag. DEMNUni: The clustering of large-scale structures in the presence of massive neutrinos.JCAP, 07:043, 2015

    work page 2015

  64. [64]

    Cosmology with massive neutrinos III: the halo mass function and an application to galaxy clusters.JCAP, 12:012, 2013

    Matteo Costanzi, Francisco Villaescusa-Navarro, Matteo Viel, Jun-Qing Xia, Stefano Borgani, Emanuele Castorina, and Emiliano Sefusatti. Cosmology with massive neutrinos III: the halo mass function and an application to galaxy clusters.JCAP, 12:012, 2013

    work page 2013

  65. [65]

    Sheth, Francisco Villaescusa-Navarro, and Matteo Viel

    Emanuele Castorina, Emiliano Sefusatti, Ravi K. Sheth, Francisco Villaescusa-Navarro, and Matteo Viel. Cosmology with massive neutrinos II: on the universality of the halo mass function and bias. JCAP, 02:049, 2014

    work page 2014

  66. [66]

    Cosmology with massive neutrinos I: towards a realistic modeling of the relation between matter, haloes and galaxies.JCAP, 03:011, 2014

    Francisco Villaescusa-Navarro, Federico Marulli, Matteo Viel, Enzo Branchini, Emanuele Castorina, Emiliano Sefusatti, and Shun Saito. Cosmology with massive neutrinos I: towards a realistic modeling of the relation between matter, haloes and galaxies.JCAP, 03:011, 2014

    work page 2014

  67. [67]

    Redshift-Space Distortions in Massive Neutrinos Cosmologies

    Francesco Verdiani, Emilio Bellini, Chiara Moretti, Emiliano Sefusatti, Carmelita Carbone, and Matteo Viel. Redshift-Space Distortions in Massive Neutrinos Cosmologies. 3 2025

    work page 2025

  68. [68]

    Effects of massive neutrinos on the large-scale structure of the universe.Monthly Notices of the Royal Astronomical Society, 418(1):346–356, 2011

    Federico Marulli, Carmelita Carbone, Matteo Viel, Lauro Moscardini, and Andrea Cimatti. Effects of massive neutrinos on the large-scale structure of the universe.Monthly Notices of the Royal Astronomical Society, 418(1):346–356, 2011

    work page 2011

  69. [69]

    Massive neutrinos and cosmology.Phys

    Julien Lesgourgues and Sergio Pastor. Massive neutrinos and cosmology.Phys. Rept., 429:307–379, 2006

    work page 2006

  70. [70]

    Andreas Ringwald and Yvonne Y. Y. Wong. Gravitational clustering of relic neutrinos and implications for their detection.JCAP, 12:005, 2004

    work page 2004

  71. [71]

    An efficient implementation of massive neutrinos in non-linear structure formation simulations.Monthly Notices of the Royal Astronomical Society, 428(4):3375–3389, 2013

    Yacine Ali-Haimoud and Simeon Bird. An efficient implementation of massive neutrinos in non-linear structure formation simulations.Monthly Notices of the Royal Astronomical Society, 428(4):3375–3389, 2013

    work page 2013

  72. [72]

    Oldengott

    Emil Brinch Holm, Stefan Zentarra, and Isabel M. Oldengott. Local clustering of relic neutrinos: comparison of kinetic field theory and the Vlasov equation.JCAP, 07:050, 2024

    work page 2024

  73. [73]

    Hotinli, Nashwan Sabti, Jaxon North, and Marc Kamionkowski

    Selim C. Hotinli, Nashwan Sabti, Jaxon North, and Marc Kamionkowski. Unveiling neutrino halos with CMB lensing.Phys. Rev. D, 108(10):103504, 2023

    work page 2023

  74. [74]

    Mass reconstruction with cmb polarization.Astrophys

    Wayne Hu and Takemi Okamoto. Mass reconstruction with cmb polarization.Astrophys. J., 574:566–574, 2002

    work page 2002

  75. [75]

    Hirata and Uros Seljak

    Christopher M. Hirata and Uros Seljak. Reconstruction of lensing from the cosmic microwave background polarization.Phys. Rev. D, 68:083002, 2003

    work page 2003

  76. [76]

    Maniyar, Yacine Ali-Ha¨ ımoud, Julien Carron, Antony Lewis, and Mathew S

    Abhishek S. Maniyar, Yacine Ali-Ha¨ ımoud, Julien Carron, Antony Lewis, and Mathew S. Madhavacheril. Quadratic estimators for CMB weak lensing.Phys. Rev. D, 103(8):083524, 2021

    work page 2021

  77. [77]

    Smith, Mathew S

    Kendrick M. Smith, Mathew S. Madhavacheril, Moritz M¨ unchmeyer, Simone Ferraro, Utkarsh Giri, and Matthew C. Johnson. KSZ tomography and the bispectrum. 10 2018

    work page 2018

  78. [78]

    Johnson, Moritz M¨ unchmeyer, and Alexandra Terrana

    Anne-Sylvie Deutsch, Emanuela Dimastrogiovanni, Matthew C. Johnson, Moritz M¨ unchmeyer, and Alexandra Terrana. Reconstruction of the remote dipole and quadrupole fields from the kinetic Sunyaev Zel’dovich and polarized Sunyaev Zel’dovich effects.Phys. Rev. D, 98(12):123501, 2018

    work page 2018

  79. [79]

    Hotinli, Kendrick M

    Selim C. Hotinli, Kendrick M. Smith, and Simone Ferraro. Velocity Reconstruction from KSZ: Measuringf N L with ACT and DESILS. 6 2025

    work page 2025

  80. [80]

    hmcode-2020: improved modelling of non-linear cosmological power spectra with baryonic feedback.Mon

    Alexander Mead, Samuel Brieden, Tilman Tr¨ oster, and Catherine Heymans. hmcode-2020: improved modelling of non-linear cosmological power spectra with baryonic feedback.Mon. Not. Roy. Astron. Soc., 502(1):1401–1422, 2021. – 25 –

    work page 2020

Showing first 80 references.