pith. sign in

arxiv: 2606.07106 · v1 · pith:E4EQOXGFnew · submitted 2026-06-05 · ✦ hep-ph · astro-ph.CO

Joint probes of dark matter annihilation from neutrino detectors and CMB targets

Ruifeng Leng , Shao-Ping Li This is my paper

Pith reviewed 2026-06-27 21:57 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.CO
keywords dark matter annihilationneutrino detectorsCMB spectral distortionseffective neutrino numberMeV-GeV dark matterSuper-Kamiokandejoint probesmodel-independent analysis
0
0 comments X

The pith

Dark matter annihilation into neutrinos can be jointly constrained by neutrino detector fluxes and CMB observables for MeV-GeV masses.

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

Neutrino detectors can observe fluxes from dark matter annihilation into neutrinos, but such signals alone leave their origin ambiguous. The paper proposes that the effective number of neutrino species and CMB spectral distortions act as independent cosmological checks on the same process. A model-independent calculation maps the parameter space where these CMB signatures overlap with the reach of Super-Kamiokande, Jiangmen Underground Neutrino Observatory, Hyper-Kamiokande, and the Deep Underground Neutrino Experiment. This overlap opens a route to cross-verify any candidate dark matter signal across astrophysical and cosmological datasets. If the windows align as described, future data from these experiments could tighten bounds on the annihilation rate in a way that neither probe achieves separately.

Core claim

Using a simple model-independent analysis, we determine the detection windows of these cosmic observables that overlap with the experimental sensitivities from the Super-Kamiokande, Jiangmen Underground Neutrino Observatory, Hyper-Kamiokande, and the Deep Underground Neutrino Experiment, showing that joint probes of large DM annihilation to neutrinos with MeV-GeV masses can be achieved by neutrino detectors and CMB experiments.

What carries the argument

Effective number of neutrino species and CMB spectral distortions as complementary observables to dark matter annihilation into neutrinos.

If this is right

  • Overlapping sensitivity windows allow combined constraints on the dark matter annihilation cross section for masses between MeV and GeV.
  • Any excess neutrino events can be checked against CMB data to test whether they share a common cosmological origin.
  • Upcoming detectors such as Hyper-Kamiokande and DUNE will extend the joint probe to a wider range of dark matter masses and rates.
  • CMB measurements provide an independent handle that reduces the chance of misidentifying astrophysical neutrino backgrounds as dark matter signals.

Where Pith is reading between the lines

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

  • The approach could be extended to other annihilation channels if they also alter N_eff or produce spectral distortions.
  • Multi-messenger consistency checks of this type might become standard for interpreting any future neutrino excesses.
  • Tighter future CMB polarization data could independently bound the same annihilation parameter space even if neutrino detectors see nothing.

Load-bearing premise

Dark matter annihilation into neutrinos produces measurable effects in the effective number of neutrino species and CMB spectral distortions that are not heavily contaminated by other cosmological sources.

What would settle it

Observation of a neutrino excess in Super-Kamiokande or Hyper-Kamiokande with no corresponding shift in the effective neutrino number or CMB spectral distortions.

read the original abstract

Dark matter (DM) annihilation into neutrinos provides a promising observational channel targeted by current and forthcoming neutrino detectors. However, the detection of such neutrino fluxes alone cannot uniquely determine their astrophysical or cosmological origin, such as the recent observations from Super-Kamiokande that hint at a small excess of electron antineutrino events. We propose that the effective number of neutrino species and the spectral distortion of the cosmic microwave background (CMB) can serve as complementary observables to probe neutrino signatures from DM annihilation. Using a simple model-independent analysis, we determine the detection windows of these cosmic observables that overlap with the experimental sensitivities from the Super-Kamiokande, Jiangmen Underground Neutrino Observatory, Hyper-Kamiokande, and the Deep Underground Neutrino Experiment, showing that joint probes of large DM annihilation to neutrinos with MeV-GeV masses can be achieved by neutrino detectors and CMB experiments.

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 proposes that the effective number of neutrino species (N_eff) and CMB spectral distortions can serve as complementary cosmological observables to direct neutrino flux measurements for identifying DM annihilation into neutrinos. Using a simple model-independent analysis, it identifies overlapping detection windows between neutrino experiments (Super-Kamiokande, Jiangmen Underground Neutrino Observatory, Hyper-Kamiokande, DUNE) and CMB experiments for MeV-GeV mass DM, enabling joint probes of such annihilation signals.

Significance. If the claimed detection windows and distortion signals are quantitatively supported, the work would strengthen multi-messenger constraints on DM by linking potential neutrino excesses to independent cosmological signatures, improving the ability to distinguish DM origins from astrophysical backgrounds.

major comments (2)
  1. [CMB spectral distortions section] The section on CMB spectral distortions and the model-independent analysis: the central claim of overlapping detection windows for spectral distortions (mu/y-type) from DM annihilation exclusively to neutrinos is unsupported. Energy injection into neutrinos after photon-neutrino decoupling (T ≲ few MeV) alters N_eff but does not directly heat the photon-baryon fluid or produce observable photon spectral distortions without pre-decoupling injection, hidden couplings, or secondary processes; no explicit calculation of non-negligible distortion amplitude is provided for neutrino-only final states. This is load-bearing for the joint-probe claim involving CMB experiments.
  2. [Detection windows analysis] The detection windows determination: the overlap between neutrino detector sensitivities and CMB spectral distortion sensitivities for the same annihilation rate is asserted but lacks quantitative demonstration that the distortion signal exceeds experimental thresholds for the MeV-GeV mass range under the neutrino-only assumption.
minor comments (2)
  1. [Methodology] Clarify the precise redshift range and decoupling assumptions used in the model-independent mapping from annihilation rate to N_eff and distortion parameters.
  2. [Results] Add explicit comparison of the derived windows to existing literature bounds on DM annihilation to neutrinos from N_eff alone.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive report and for identifying key points that require clarification. We address each major comment below and indicate where revisions will be made to the manuscript.

read point-by-point responses

  1. Referee: [CMB spectral distortions section] The section on CMB spectral distortions and the model-independent analysis: the central claim of overlapping detection windows for spectral distortions (mu/y-type) from DM annihilation exclusively to neutrinos is unsupported. Energy injection into neutrinos after photon-neutrino decoupling (T ≲ few MeV) alters N_eff but does not directly heat the photon-baryon fluid or produce observable photon spectral distortions without pre-decoupling injection, hidden couplings, or secondary processes; no explicit calculation of non-negligible distortion amplitude is provided for neutrino-only final states. This is load-bearing for the joint-probe claim involving CMB experiments.

    Authors: We agree with the referee that neutrino-only energy injection after photon-neutrino decoupling primarily modifies N_eff and does not generate direct mu- or y-type spectral distortions in the photon fluid without additional mechanisms. The manuscript's discussion of spectral distortions was intended to cover the general case of early-universe injection (pre-decoupling) or possible secondary effects, but we did not provide an explicit calculation of the distortion amplitude for the neutrino-only final state in the MeV-GeV range. We will revise this section to (i) clearly separate the N_eff and spectral-distortion regimes, (ii) state that distortions are negligible for post-decoupling neutrino injection, and (iii) either remove the overlapping-window claim for spectral distortions or add the requested quantitative estimate showing the amplitude falls below observational thresholds. This constitutes a partial revision of the joint-probe narrative. revision: partial

  2. Referee: [Detection windows analysis] The detection windows determination: the overlap between neutrino detector sensitivities and CMB spectral distortion sensitivities for the same annihilation rate is asserted but lacks quantitative demonstration that the distortion signal exceeds experimental thresholds for the MeV-GeV mass range under the neutrino-only assumption.

    Authors: The referee is correct that the manuscript asserts overlap without a dedicated quantitative comparison of the expected distortion amplitude against experimental sensitivity for the neutrino-only channel. We will add an explicit calculation (or reference to standard distortion templates) demonstrating that the photon distortion signal remains below current and projected thresholds for the relevant masses and annihilation rates. The revised detection-window figures and text will reflect this result, restricting the CMB spectral-distortion contribution to cases where it is actually observable. revision: yes

Circularity Check

0 steps flagged

No circularity: model-independent overlap analysis uses standard observables

full rationale

The paper performs a model-independent analysis to identify overlapping detection windows between neutrino detector sensitivities and standard cosmological observables (N_eff, CMB spectral distortions) for DM annihilation to neutrinos. No equations or steps reduce by construction to author-defined fits, self-citations that bear the central load, or renamed known results. The derivation chain relies on external experimental sensitivities and established cosmological effects without self-referential definitions or parameter predictions that are forced by the inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review; no specific free parameters, axioms, or invented entities can be identified from the provided text. The proposal appears to rest on standard dark matter annihilation and cosmological models.

pith-pipeline@v0.9.1-grok · 5677 in / 1033 out tokens · 19558 ms · 2026-06-27T21:57:59.692579+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

82 extracted references · 37 linked inside Pith

  1. [1]

    Akita, G

    K. Akita, G. Lambiase, M. Niibo, and M. Yamaguchi,Neutrino lines from MeV dark matter annihilation and decay in JUNO,JCAP10(2022) 097, [arXiv:2206.06755]. [7]JUNOCollaboration, A. Abusleme et al.,JUNO sensitivity to the annihilation of MeV dark matter in the galactic halo,JCAP09(2023) 001, [arXiv:2306.09567]. [8]Super-KamiokandeCollaboration, J. Hosaka et...

    arXiv 2022

  2. [2]

    Olivares-Del Campo, C

    A. Olivares-Del Campo, C. Bœhm, S. Palomares-Ruiz, and S. Pascoli,Dark matter-neutrino interactions through the lens of their cosmological implications,Phys. Rev. D97(2018), no. 7 075039, [arXiv:1711.05283]. [13]Hyper-KamiokandeCollaboration, K. Abe et al.,Hyper-Kamiokande Design Report, arXiv:1805.04163. [14]DUNECollaboration, R. Acciarri et al.,Long-Bas...

    Pith/arXiv arXiv 2018

  3. [3]

    Capozzi, S

    F. Capozzi, S. W. Li, G. Zhu, and J. F. Beacom,DUNE as the Next-Generation Solar Neutrino Experiment,Phys. Rev. Lett.123(2019), no. 13 131803, [arXiv:1808.08232]. [16]IceCubeCollaboration, M. G. Aartsen et al.,The IceCube Neutrino Observatory: Instrumentation and Online Systems,JINST12(2017), no. 03 P03012, [arXiv:1612.05093]. [Erratum: JINST 19, E05001 (...

    arXiv 2019

  4. [4]

    Harada,Review of diffuse sn neutrino background, June, 2024

    M. Harada,Review of diffuse sn neutrino background, June, 2024

    2024

  5. [5]

    Santos, M

    A. Santos, M. Harada, and Y . Kanemura,New limits on the low-energy astrophysical electron antineutrinos at sk-gd experiment, June, 2024

    2024

  6. [6]

    Rogly,Overview of the model-dependent approach for the diffuse supernova neutrino background search with the sk-gd experiment, June, 2024

    R. Rogly,Overview of the model-dependent approach for the diffuse supernova neutrino background search with the sk-gd experiment, June, 2024

    2024

  7. [7]

    Beauch ˆene,Diffuse supernova neutrino background: Insights from super-kamiokande & prospects with hyper- kamiokande, June, 2024

    A. Beauch ˆene,Diffuse supernova neutrino background: Insights from super-kamiokande & prospects with hyper- kamiokande, June, 2024. – 22 –

    2024

  8. [8]

    Kotake, K

    K. Kotake, K. Sato, and K. Takahashi,Explosion mechanism, neutrino burst, and gravitational wave in core-collapse supernovae,Rept. Prog. Phys.69(2006) 971–1144, [astro-ph/0509456]

    Pith/arXiv arXiv 2006

  9. [9]

    Mirizzi, I

    A. Mirizzi, I. Tamborra, H.-T. Janka, N. Saviano, K. Scholberg, R. Bollig, L. Hudepohl, and S. Chakraborty,Supernova Neutrinos: Production, Oscillations and Detection,Riv. Nuovo Cim.39 (2016), no. 1-2 1–112, [arXiv:1508.00785]

    Pith/arXiv arXiv 2016

  10. [10]

    Horiuchi and J

    S. Horiuchi and J. P. Kneller,What can be learned from a future supernova neutrino detection?,J. Phys. G45(2018), no. 4 043002, [arXiv:1709.01515]

    Pith/arXiv arXiv 2018

  11. [11]

    Palomares-Ruiz and S

    S. Palomares-Ruiz and S. Pascoli,Testing MeV dark matter with neutrino detectors,Phys. Rev. D77 (2008) 025025, [arXiv:0710.5420]

    Pith/arXiv arXiv 2008

  12. [12]

    C. M. Ho and R. J. Scherrer,Limits on MeV Dark Matter from the Effective Number of Neutrinos, Phys. Rev. D87(2013), no. 2 023505, [arXiv:1208.4347]

    Pith/arXiv arXiv 2013

  13. [13]

    Boehm, M

    C. Boehm, M. J. Dolan, and C. McCabe,A Lower Bound on the Mass of Cold Thermal Dark Matter from Planck,JCAP08(2013) 041, [arXiv:1303.6270]

    Pith/arXiv arXiv 2013

  14. [14]

    C. A. Arg ¨uelles, A. Diaz, A. Kheirandish, A. Olivares-Del-Campo, I. Safa, and A. C. Vincent,Dark matter annihilation to neutrinos,Rev. Mod. Phys.93(2021), no. 3 035007, [arXiv:1912.09486]

    arXiv 2021

  15. [15]

    Sabti, J

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

    arXiv 2020

  16. [16]

    Kanemura, S.-P

    S. Kanemura, S.-P. Li, and D. Nanda,Bounds and detection of MeV-scale dark matter annihilation to neutrinos,Phys. Rev. D112(2025), no. 3 L031702, [arXiv:2506.04568]

    arXiv 2025

  17. [17]

    Steigman, B

    G. Steigman, B. Dasgupta, and J. F. Beacom,Precise Relic WIMP Abundance and its Impact on Searches for Dark Matter Annihilation,Phys. Rev. D86(2012) 023506, [arXiv:1204.3622]

    Pith/arXiv arXiv 2012

  18. [18]

    Chu and J

    X. Chu and J. Pradler,Minimal mass of thermal dark matter and the viability of millicharged particles affecting 21-cm cosmology,Phys. Rev. D109(2024), no. 10 103510, [arXiv:2310.06611]

    arXiv 2024

  19. [19]

    Granelli, S

    A. Granelli, S. Pascoli, and S. Rosauro-Alcaraz,Dark Matter Interpretation of the Super-Kamiokande Antineutrino Excess and Predictions for JUNO,arXiv:2605.20162

    Pith/arXiv arXiv

  20. [20]

    M. Endo, Y . Mura, and T. Tsuji,Dark Matter Interpretation of the Super-Kamiokande Antineutrino Excess inU(1) Lµ−Lτ model,arXiv:2605.28275

    Pith/arXiv arXiv

  21. [21]

    Mangano, G

    G. Mangano, G. Miele, S. Pastor, and M. Peloso,A Precision calculation of the effective number of cosmological neutrinos,Phys. Lett. B534(2002) 8–16, [astro-ph/0111408]

    Pith/arXiv arXiv 2002

  22. [22]

    Mangano, G

    G. Mangano, G. Miele, S. Pastor, T. Pinto, O. Pisanti, and P. D. Serpico,Relic neutrino decoupling including flavor oscillations,Nucl. Phys. B729(2005) 221–234, [hep-ph/0506164]

    Pith/arXiv arXiv 2005

  23. [23]

    P. F. de Salas and S. Pastor,Relic neutrino decoupling with flavour oscillations revisited,JCAP07 (2016) 051, [arXiv:1606.06986]

    Pith/arXiv arXiv 2016

  24. [24]

    Escudero,Neutrino decoupling beyond the Standard Model: CMB constraints on the Dark Matter mass with a fast and preciseN eff evaluation,JCAP02(2019) 007, [arXiv:1812.05605]

    M. Escudero,Neutrino decoupling beyond the Standard Model: CMB constraints on the Dark Matter mass with a fast and preciseN eff evaluation,JCAP02(2019) 007, [arXiv:1812.05605]

    arXiv 2019

  25. [25]

    J. J. Bennett, G. Buldgen, P. F. De Salas, M. Drewes, S. Gariazzo, S. Pastor, and Y . Y . Y . Wong, Towards a precision calculation ofNeff in the Standard Model II: Neutrino decoupling in the presence of flavour oscillations and finite-temperature QED,JCAP04(2021) 073, [arXiv:2012.02726]. – 23 –

    arXiv 2021

  26. [26]

    Escudero Abenza,Precision early universe thermodynamics made simple:N eff and neutrino decoupling in the Standard Model and beyond,JCAP05(2020) 048, [arXiv:2001.04466]

    M. Escudero Abenza,Precision early universe thermodynamics made simple:N eff and neutrino decoupling in the Standard Model and beyond,JCAP05(2020) 048, [arXiv:2001.04466]

    arXiv 2020

  27. [27]

    Cielo, M

    M. Cielo, M. Escudero, G. Mangano, and O. Pisanti,Neff in the Standard Model at NLO is 3.043, Phys. Rev. D108(2023), no. 12 L121301, [arXiv:2306.05460]

    arXiv 2023

  28. [28]

    Burigana, L

    C. Burigana, L. Danese, and G. De Zotti,Formation and evolution of early distortions of the microwave background spectrum - A numerical study,Astron. Astrophys.246(1991), no. 1 49–58

    1991

  29. [29]

    Hu and J

    W. Hu and J. Silk,Thermalization and spectral distortions of the cosmic background radiation, Phys. Rev. D48(1993) 485–502

    1993

  30. [30]

    Li and J

    S.-P. Li and J. Chluba,Neutrinogenic CMB spectral distortions,Phys. Rev. D113(2026), no. 4 043504, [arXiv:2510.04684]

    arXiv 2026

  31. [31]

    Khatri and R

    R. Khatri and R. A. Sunyaev,Beyond y andµ: the shape of the CMB spectral distortions in the intermediate epoch,1.5×10 4 < z <2×10 5,JCAP09(2012) 016, [arXiv:1207.6654]

    Pith/arXiv arXiv 2012

  32. [32]

    S. K. Acharya and R. Khatri,Rich structure of non-thermal relativistic CMB spectral distortions from high energy particle cascades at redshiftsz≲2×10 5,Phys. Rev. D99(2019), no. 4 043520, [arXiv:1808.02897]

    Pith/arXiv arXiv 2019

  33. [33]

    Chluba and R

    J. Chluba and R. A. Sunyaev,The evolution of CMB spectral distortions in the early Universe,Mon. Not. Roy. Astron. Soc.419(2012) 1294–1314, [arXiv:1109.6552]

    Pith/arXiv arXiv 2012

  34. [34]

    J. C. Mather et al.,Measurement of the Cosmic Microwave Background spectrum by the COBE FIRAS instrument,Astrophys. J.420(1994) 439–444

    1994

  35. [35]

    D. J. Fixsen, E. S. Cheng, J. M. Gales, J. C. Mather, R. A. Shafer, and E. L. Wright,The Cosmic Microwave Background spectrum from the full COBE FIRAS data set,Astrophys. J.473(1996) 576, [astro-ph/9605054]

    Pith/arXiv arXiv 1996

  36. [36]

    Bianchini and G

    F. Bianchini and G. Fabbian,CMB spectral distortions revisited: A new take onµdistortions and primordial non-Gaussianities from FIRAS data,Phys. Rev. D106(2022), no. 6 063527, [arXiv:2206.02762]

    arXiv 2022

  37. [37]

    Sabyr, G

    A. Sabyr, G. Fabbian, J. C. Hill, and F. Bianchini,A new constraint on they-distortion with FIRAS: robustness of component separation methods,arXiv:2508.04593

    arXiv

  38. [38]

    B. Maffei et al.,BISOU: A balloon project to measure the CMB spectral distortions, in16th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Astrophysics and Relativistic Field Theories, 10, 2021.arXiv:2111.00246

    arXiv 2021

  39. [39]

    Masi et al.,The cosmic monopole observer (cosmo),arXiv:2110.12254

    S. Masi et al.,The cosmic monopole observer (cosmo),arXiv:2110.12254

    arXiv

  40. [40]

    Alonso-Arias et al.,A Microwave Blackbody Target for Cosmic Microwave Background Spectral Measurements in the 10-20GHz range,arXiv:2309.07320

    P. Alonso-Arias et al.,A Microwave Blackbody Target for Cosmic Microwave Background Spectral Measurements in the 10-20GHz range,arXiv:2309.07320

    arXiv

  41. [41]

    Sabyr, C

    A. Sabyr, C. Sierra, J. C. Hill, and J. J. McMahon,SPECTER: An Instrument Concept for CMB Spectral Distortion Measurements with Enhanced Sensitivity,arXiv:2409.12188

    arXiv

  42. [42]

    Kogut et al.,The Primordial Inflation Explorer (PIXIE): A Nulling Polarimeter for Cosmic Microwave Background Observations,JCAP07(2011) 025, [arXiv:1105.2044]

    A. Kogut et al.,The Primordial Inflation Explorer (PIXIE): A Nulling Polarimeter for Cosmic Microwave Background Observations,JCAP07(2011) 025, [arXiv:1105.2044]

    Pith/arXiv arXiv 2011

  43. [43]

    Kogut et al.,The Primordial Inflation Explorer (PIXIE): mission design and science goals,JCAP 04(2025) 020, [arXiv:2405.20403]

    A. Kogut et al.,The Primordial Inflation Explorer (PIXIE): mission design and science goals,JCAP 04(2025) 020, [arXiv:2405.20403]

    arXiv 2025

  44. [44]

    Kogut, M

    A. Kogut, M. H. Abitbol, J. Chluba, J. Delabrouille, D. Fixsen, J. C. Hill, S. P. Patil, and A. Rotti, CMB Spectral Distortions: Status and Prospects,Bull. Am. Astron. Soc.51(2019), no. 7 113, [arXiv:1907.13195]. – 24 –

    arXiv 2019

  45. [45]

    Chluba et al.,New horizons in cosmology with spectral distortions of the cosmic microwave background,Exper

    J. Chluba et al.,New horizons in cosmology with spectral distortions of the cosmic microwave background,Exper. Astron.51(2021), no. 3 1515–1554, [arXiv:1909.01593]

    arXiv 2021

  46. [46]

    Batell, T

    B. Batell, T. Han, D. McKeen, and B. Shams Es Haghi,Thermal Dark Matter Through the Dirac Neutrino Portal,Phys. Rev. D97(2018), no. 7 075016, [arXiv:1709.07001]

    Pith/arXiv arXiv 2018

  47. [47]

    Ballett, M

    P. Ballett, M. Hostert, and S. Pascoli,Dark Neutrinos and a Three Portal Connection to the Standard Model,Phys. Rev. D101(2020), no. 11 115025, [arXiv:1903.07589]

    arXiv 2020

  48. [48]

    Blennow, E

    M. Blennow, E. Fernandez-Martinez, A. Olivares-Del Campo, S. Pascoli, S. Rosauro-Alcaraz, and A. V . Titov,Neutrino Portals to Dark Matter,Eur. Phys. J. C79(2019), no. 7 555, [arXiv:1903.00006]

    arXiv 2019

  49. [49]

    Li and X.-J

    S.-P. Li and X.-J. Xu,Dark matter produced from right-handed neutrinos,JCAP06(2023) 047, [arXiv:2212.09109]

    arXiv 2023

  50. [50]

    J. L. Feng, A. Rajaraman, and F. Takayama,Superweakly interacting massive particles,Phys. Rev. Lett.91(2003) 011302, [hep-ph/0302215]

    Pith/arXiv arXiv 2003

  51. [51]

    J. L. Feng, A. Rajaraman, and F. Takayama,SuperWIMP dark matter signals from the early universe,Phys. Rev. D68(2003) 063504, [hep-ph/0306024]

    Pith/arXiv arXiv 2003

  52. [52]

    Cohen, D

    T. Cohen, D. E. Morrissey, and A. Pierce,Changes in Dark Matter Properties After Freeze-Out, Phys. Rev. D78(2008) 111701, [arXiv:0808.3994]

    Pith/arXiv arXiv 2008

  53. [53]

    M. J. Baker, J. Kopp, and A. J. Long,Filtered Dark Matter at a First Order Phase Transition,Phys. Rev. Lett.125(2020), no. 15 151102, [arXiv:1912.02830]

    arXiv 2020

  54. [54]

    Wong and K.-P

    X.-R. Wong and K.-P. Xie,Freeze-in of WIMP dark matter,Phys. Rev. D108(2023), no. 5 055035, [arXiv:2304.00908]. [71]PlanckCollaboration, N. Aghanim et al.,Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys.641(2020) A6, [arXiv:1807.06209]. [Erratum: Astron.Astrophys. 652, C4 (2021)]

    arXiv 2023

  55. [55]

    Hambye, M

    T. Hambye, M. Hufnagel, and M. Lucca,Cosmological constraints on the decay of heavy relics into neutrinos,JCAP05(2022), no. 05 033, [arXiv:2112.09137]

    arXiv 2022

  56. [56]

    Li and X.-J

    S.-P. Li and X.-J. Xu,N ef f constraints on light mediators coupled to neutrinos: the dilution-resistant effect,JHEP10(2023) 012, [arXiv:2307.13967]

    arXiv 2023

  57. [57]

    Bianco, P

    S. Bianco, P. F. Depta, J. Frerick, T. Hambye, M. Hufnagel, and K. Schmidt-Hoberg,Photo- and Hadrodisintegration constraints on massive relics decaying into neutrinos,arXiv:2505.01492

    arXiv

  58. [58]

    Chang, S

    S. Chang, S. Ganguly, T. H. Jung, T.-S. Park, and C. S. Shin,Constraining MeV to 10 GeV Majorons by big bang nucleosynthesis,Phys. Rev. D110(2024), no. 1 015019, [arXiv:2401.00687]

    arXiv 2024

  59. [59]

    J. A. Formaggio and G. P. Zeller,From eV to EeV: Neutrino Cross Sections Across Energy Scales, Rev. Mod. Phys.84(2012) 1307–1341, [arXiv:1305.7513]

    Pith/arXiv arXiv 2012

  60. [60]

    Borsanyi et al.,Calculation of the axion mass based on high-temperature lattice quantum chromodynamics,Nature539(2016), no

    S. Borsanyi et al.,Calculation of the axion mass based on high-temperature lattice quantum chromodynamics,Nature539(2016), no. 7627 69–71, [arXiv:1606.07494]

    Pith/arXiv arXiv 2016

  61. [61]

    Kawasaki and T

    M. Kawasaki and T. Moroi,Gravitino decay into a neutrino and a sneutrino in the inflationary universe,Phys. Lett. B346(1995) 27–34, [hep-ph/9408321]

    Pith/arXiv arXiv 1995

  62. [62]

    S. K. Acharya and R. Khatri,Constraints onN eff of high energy non-thermal neutrino injections uptoz∼10 8 from CMB spectral distortions and abundance of light elements,JCAP11(2020) 011, [arXiv:2007.06596]. – 25 –

    arXiv 2020

  63. [63]

    Kanzaki, M

    T. Kanzaki, M. Kawasaki, K. Kohri, and T. Moroi,Cosmological Constraints on Neutrino Injection, Phys. Rev. D76(2007) 105017, [arXiv:0705.1200]

    Pith/arXiv arXiv 2007

  64. [64]

    Gratsias, R

    J. Gratsias, R. J. Scherrer, and D. N. Spergel,Indirect photofission of light elements from high-energy neutrinos in the early universe,Phys. Lett. B262(1991) 298–302

    1991

  65. [65]

    A. A. de Laix and R. J. Scherrer,Improved cosmological constraints on neutrino producing decaying particles,Phys. Rev. D48(1993) 562–566

    1993

  66. [66]

    McDonald, R

    P. McDonald, R. J. Scherrer, and T. P. Walker,Cosmic microwave background constraint on residual annihilations of relic particles,Phys. Rev. D63(2001) 023001, [astro-ph/0008134]

    Pith/arXiv arXiv 2001

  67. [67]

    G. R. Blumenthal and R. J. Gould,Bremsstrahlung, synchrotron radiation, and compton scattering of high-energy electrons traversing dilute gases,Rev. Mod. Phys.42(1970) 237–270

    1970

  68. [68]

    Chen and M

    X.-L. Chen and M. Kamionkowski,Particle decays during the cosmic dark ages,Phys. Rev. D70 (2004) 043502, [astro-ph/0310473]

    Pith/arXiv arXiv 2004

  69. [69]

    Padmanabhan and D

    N. Padmanabhan and D. P. Finkbeiner,Detecting dark matter annihilation with CMB polarization: Signatures and experimental prospects,Phys. Rev. D72(2005) 023508, [astro-ph/0503486]

    Pith/arXiv arXiv 2005

  70. [70]

    Hannestad,Oscillation effects on neutrino decoupling in the early universe,Phys

    S. Hannestad,Oscillation effects on neutrino decoupling in the early universe,Phys. Rev. D65 (2002) 083006, [astro-ph/0111423]

    Pith/arXiv arXiv 2002

  71. [71]

    A. D. Dolgov, S. H. Hansen, S. Pastor, S. T. Petcov, G. G. Raffelt, and D. V . Semikoz,Cosmological bounds on neutrino degeneracy improved by flavor oscillations,Nucl. Phys. B632(2002) 363–382, [hep-ph/0201287]

    Pith/arXiv arXiv 2002

  72. [72]

    Li,Observability of CMB spectrum distortions from dark matter annihilation,JCAP07(2024) 019, [arXiv:2402.16708]

    S.-P. Li,Observability of CMB spectrum distortions from dark matter annihilation,JCAP07(2024) 019, [arXiv:2402.16708]

    arXiv 2024

  73. [73]

    R. A. Sunyaev and Y . B. Zeldovich,The Interaction of matter and radiation in the hot model of the universe,Astrophys. Space Sci.7(1970) 20–30

    1970

  74. [74]

    Khatri and R

    R. Khatri and R. A. Sunyaev,Creation of the CMB spectrum: precise analytic solutions for the blackbody photosphere,JCAP06(2012) 038, [arXiv:1203.2601]

    Pith/arXiv arXiv 2012

  75. [75]

    Chluba,Refined approximations for the distortion visibility function andµ-type spectral distortions,Mon

    J. Chluba,Refined approximations for the distortion visibility function andµ-type spectral distortions,Mon. Not. Roy. Astron. Soc.440(2014), no. 3 2544–2563, [arXiv:1312.6030]

    Pith/arXiv arXiv 2014

  76. [76]

    Chluba,Which spectral distortions doesΛCDM actually predict?,Mon

    J. Chluba,Which spectral distortions doesΛCDM actually predict?,Mon. Not. Roy. Astron. Soc. 460(2016), no. 1 227–239, [arXiv:1603.02496]

    Pith/arXiv arXiv 2016

  77. [77]

    Horiuchi, J

    S. Horiuchi, J. F. Beacom, and E. Dwek,The Diffuse Supernova Neutrino Background is detectable in Super-Kamiokande,Phys. Rev. D79(2009) 083013, [arXiv:0812.3157]

    Pith/arXiv arXiv 2009

  78. [78]

    N. F. Bell, M. J. Dolan, and S. Robles,Searching for Sub-GeV Dark Matter in the Galactic Centre using Hyper-Kamiokande,JCAP09(2020) 019, [arXiv:2005.01950]

    arXiv 2020

  79. [79]

    Honda, M

    M. Honda, M. Sajjad Athar, T. Kajita, K. Kasahara, and S. Midorikawa,Atmospheric neutrino flux calculation using the NRLMSISE-00 atmospheric model,Phys. Rev. D92(2015), no. 2 023004, [arXiv:1502.03916]. [97]Simons ObservatoryCollaboration, P. Ade et al.,The Simons Observatory: Science goals and forecasts,JCAP02(2019) 056, [arXiv:1808.07445]. [98]Simons Ob...

    Pith/arXiv arXiv 2015

  80. [80]

    K. M. Nollett and G. Steigman,BBN And The CMB Constrain Neutrino Coupled Light WIMPs, Phys. Rev. D91(2015), no. 8 083505, [arXiv:1411.6005]

    Pith/arXiv arXiv 2015

Showing first 80 references.