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Probing a diffuse flux of axion-like particles from galactic supernovae with neutrino water Cherenkov detectors

T0 review · 2 major / 3 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read MeV-mass axion-like particles from galactic supernovae form a diffuse flux detectable by water Cherenkov detectors, and Super-Kamiokande data exclude proton couplings of roughly $2\times10^{-5}$ to $2\times10^{-4}$ for masses of 1–70 MeV.

desk verdict Good idea with a new exclusion claim, but a missing Jacobian in Eq. (14) makes the bound unreliable until the cross section is corrected. read the letter →

arxiv 2412.09595 v4 pith:UT3WGV46 submitted 2024-12-12 hep-ph astro-ph.CO

David Alonso-González , David Cerdeño , Marina Cermeño , Andres D. Perez This is my paper · ORCID
classification hep-phastro-ph.CO
keywords axion-likeparticlesMeVALPscore-collapsesupernovaediffusegalacticfluxwaterCherenkovdetectorsALP-protoncouplingtrappingregimeSuper-Kamiokande
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

MeV-mass axion-like particles produced in core-collapse supernovae would not arrive as a single burst: because they leave the proto-neutron star with a spread of semi-relativistic speeds, their arrival times stretch over hundreds to thousands of years, so the roughly two supernovae per century in the Milky Way produce a near-steady diffuse galactic flux. The paper shows that this flux can be detected in neutrino water Cherenkov detectors through $a p \to p \gamma$ scattering on free protons, yielding photons in the tens-of-MeV range where backgrounds are small. Using the first four phases of Super-Kamiokande data, the authors exclude ALP-proton couplings between about $2\times10^{-5}$ and $2\times10^{-4}$ for ALP masses of 1–70 MeV, a band one order of magnitude above the SN 1987A cooling bounds. This would be the first direct probe of the trapping regime of MeV ALPs through a diffuse galactic supernova flux, and the projected Hyper-Kamiokande sensitivity would extend the reach down to couplings near $\sim 10^{-5}$.

What carries the argument

The load-bearing mechanism is the arrival-time spread: ALPs with $m_a \gtrsim 1$ MeV leave the proto-NS with an order-one velocity spread, giving arrival-time differences $\Delta t \simeq d/\bar v\,\delta v \sim 5\times10^2$–$5\times10^3$ years for Galactic Center distances, so the Milky Way supernova rate of about two per century makes the flux from roughly ten to one hundred supernovae overlap into a steady diffuse galactic component. The detection mechanism is the inverse photo-production process $a p \to p \gamma$, whose photon energy is fixed by two-body kinematics and falls near the ALP energy, in the tens-of-MeV range; in water Cherenkov detectors a photon is reconstructed almost like a positron, so the same signal region used for the diffuse supernova neutrino background applies. Production is computed from nucleon-nucleon bremsstrahlung and pion conversion, with reabsorption through $NN a \to NN$ and $N a \to N\pi$ and gravitational redshift included.

What would settle it

Recompute the diffuse ALP flux using a mass-weighted distribution of supernova progenitor profiles rather than the single 18-solar-mass profile; if the resulting flux at Earth is lower by more than about a factor of 2.5, the claimed Super-Kamiokande exclusion no longer reaches the stated couplings.

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Extended reading notes

Core claim

The authors' central claim is that ALPs coupled to protons, with masses in the 1–70 MeV range, are produced in proto-neutron star interiors by nucleon-nucleon bremsstrahlung and pion conversion, and that enough of them escape even in the trapping regime to make a detectable diffuse galactic flux. The flux is anisotropic and peaked toward the Galactic Center. Comparing the expected photon events from $a p \to p \gamma$ with the observed Super-Kamiokande event rates in the reconstructed-energy window 16–80 MeV, they find that the measured data are consistent with background, so the ALP signal is excluded for couplings of roughly $2\times10^{-5}$ to $2\times10^{-4}$ across 1–70 MeV. They project that Hyper-Kamiokande, with a $187\times10$ kton-year exposure, would improve that bound by up to a factor of 2.5.

Load-bearing premise

The calculation assumes every galactic core-collapse supernova emits ALPs like the same 18-solar-mass proto-neutron star profile evaluated one second after bounce; if the population-averaged flux is lower, the excluded coupling region shrinks.

Editorial extensions

If this is right

  • The SN 1987A cooling bounds, which lose sensitivity above couplings of roughly $10^{-6}$, are now supplemented by a flux-based exclusion that covers the trapping regime for $m_a=1$–70 MeV.
  • Hyper-Kamiokande should exclude couplings down to about $10^{-5}$ for $m_a=1$–50 MeV, cutting the allowed region above the upper cooling bound by up to a factor of 2.5.
  • The constraints degrade sharply outside $m_a=1$–70 MeV: below 1 MeV the steady-flux assumption fails, and above 70 MeV the SK energy window and the production suppression kill the signal.
  • The four Super-K phases combined give limits only slightly stronger than SK-IV alone, so the result is driven by the SK-IV exposure.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Beyond the paper, the same arrival-time argument should apply to any long-lived MeV-scale particle with nucleon couplings, so water Cherenkov detectors become a generic telescope for semi-relativistic dark-sector fluxes from galactic supernovae.
  • Because the diffuse flux is anisotropic and peaked toward the Galactic Center, a directional or angular-template analysis could separate it from the isotropic diffuse supernova neutrino background and strengthen the limit.
  • The paper notes that oxygen de-excitation photons from ALP scattering would outnumber the $a p \to p \gamma$ signal by two orders of magnitude; a dedicated low-energy analysis near the detector threshold could therefore probe lower couplings if the spallation background can be controlled.
  • A single nearby galactic supernova during the Hyper-Kamiokande era would break the steady-flux assumption on human timescales and provide a time-resolved check of the production spectrum used here.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 3 minor

Summary. The paper proposes that MeV-scale axion-like particles (ALPs) produced in the trapping regime of core-collapse supernovae build up a diffuse galactic flux, and that this flux can be detected in water Cherenkov detectors through a p -> p gamma interactions. Using an 18 solar-mass proto-neutron-star profile at 1 s after bounce, an emission window of 0.5-2 s, and the galactic supernova distribution, the authors compute the diffuse ALP flux. They then use Super-Kamiokande DSNB search data (SK-I through SK-IV, reconstructed energies 16-80 MeV) to set a 95% C.L. exclusion in the (gap, ma) plane, and give a projected Hyper-Kamiokande sensitivity. The headline result is a new excluded band for ma ~ 1-70 MeV and gap ~ 2e-5 to 2e-4, above the SN 1987A cooling bounds.

Significance. If the flux normalization is correct, this would be a genuinely new probe of the trapping regime of MeV ALPs, complementary to SN 1987A cooling limits, solar-axion searches, and SNO bounds. The paper is commendably explicit: the production and absorption formalism follows Refs. [27,28], the galactic-flux convolution is written out, the ALP-proton cross section is given in closed form, and the statistical treatment is relegated to an appendix with enough detail to reproduce the limit. I also checked the phase-space normalization of Eq. (14): the apparent absence of a Jacobian is not an error, because after the angular integral over the energy-conservation delta the E_gamma/E_f factors cancel with |d(E_a+m_p-E_f-E_gamma)/d cos(theta)|, leaving exactly |M|^2/(32*pi*|p_a|^2*m_p). The main risk to the central claim is therefore not the cross-section normalization but the normalization of the diffuse galactic flux itself, which rests on a single progenitor profile and on a marginal steady-flux approximation at the low-mass edge.

major comments (2)
  1. [Section III, 'For simplicity...' and Fig. 4] The exclusion contour is computed from a single 18 solar-mass proto-neutron-star profile, although the text acknowledges that most galactic progenitors are lighter and have temperatures and densities about 20% lower, while a minority are hotter. Since the ALP production rate and the absorption optical depth depend steeply on temperature and density (through Boltzmann-type factors), a 20% change in the profile can translate into an O(1) or larger change in the predicted photon counts. The quoted ~30% uncertainty from the galactic supernova rate does not cover this systematic. Because the limit sets the coupling where the predicted signal crosses the Super-Kamiokande background, the boundary of the pink band in Fig. 4 will move with this normalization. I request a bracketing estimate: recompute the flux, and if possible the contour, using a lower-mass profile from the same simulation set, or state explicitly how the contour shifts under a factor-of-two flux rescaling. Without this, the claimed one-order-of-magnitude exclusion is not quantitatively robust.
  2. [Section III, 'It is important to remark...' and Fig. 4] At ma ~ 1 MeV the arrival-time spread is only about 500 years, and with a galactic supernova rate of roughly 2 per century the expected number of overlapping bursts is only about eight to ten. The diffuse flux is then a Poisson sum with fluctuations of order 30%, not a steady background. The analysis nevertheless includes ma = 1 MeV in the excluded range and in Fig. 4. Either the claimed mass range should start where the overlap is clearly sufficient, or the Poisson variance from the finite number of contributing supernovae should be propagated into the limit. This directly affects the low-mass edge of the abstract's central claim.
minor comments (3)
  1. [Eq. (14) and surrounding text] To help readers and to preempt the Jacobian question, add one sentence after Eq. (14) showing that the displayed form follows from the two-body phase space after the photon-angle integration: the E_gamma/E_f factor from the phase space cancels the Jacobian |d(E_a+m_p-E_f-E_gamma)/d cos(theta)| = q E_gamma/E_f. The formula is correct, but a brief derivation would make this transparent.
  2. [Section III and Fig. 1] The notation alternates between ga and gap in a confusing way; for example, the text says 'we fixed the ALP-proton coupling to ga = 10^-5' even though ga = m_N/f_a and gap = ga Cap with Cap = -0.47. Please define both quantities consistently and use the same symbol for the constrained coupling shown on the vertical axis of Fig. 4.
  3. [Appendix B] The likelihood treatment fixes the background to the Horiuchi+09 DSNB model without profiling over background normalization or energy-scale nuisance parameters. This is probably acceptable for a first constraint, but it should be stated as a limitation, since the Super-Kamiokande observed spectrum has its own uncertainties.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the ALP flux is taken from external SN simulations, and Super-Kamiokande data are used only to set limits, not to fit the claimed exclusion.

full rationale

The paper's central claim is a new exclusion in ALP parameter space. The derivation chain is: (i) adopt an external 18-solar-mass proto-neutron-star profile from Ref. [24] and ALP production/absorption rates from Ref. [28]; (ii) compute a diffuse galactic flux by weighting the resulting spectral fluence with an external galactic SN rate model; (iii) compute the detection rate using a perturbative cross section for a p -> p gamma; and (iv) compare this predicted signal with published Super-Kamiokande event counts via a profiled log-likelihood. None of these steps fits the target result from the data. The benchmark couplings Cap = -0.47 and Can = 0 are fixed before comparison, not adjusted to improve agreement. The SK data enter only as observed counts and expected backgrounds, so the exclusion contour is a genuine limit rather than a re-labeling of fitted inputs. There are no load-bearing self-citations: the cited SN simulation and ALP emissivity works are by other authors, and the paper's own statistical procedure is a standard likelihood ratio. The possible omission of a phase-space Jacobian in Eq. (14), if real, would be a physics/correctness error in the cross-section normalization, not a circularity, because it does not make the predicted signal equivalent to the input data or to the fitted parameters. The stated progenitor-profile uncertainties and the steady-flux assumption are caveats about the robustness of the flux prediction, not circularity. Overall, the derivation is self-contained against external benchmarks and the claimed exclusion has independent content.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central prediction rests on five assumptions: the adopted SN temperature/density profiles and emission window, the validity of ignoring ALP backreaction, the long-lived ALP condition, the galactic SN rate model, and the statistical asymptotic. None of these are derived by the paper; the first two carry the largest uncertainty and are not propagated into the exclusion contour.

free parameters (3)
  • SN emission time window (tmin, tmax) = 0.5-2.0 s
    Chosen in Section III to match the period when the 18 M_sun proto-NS profiles from Ref [24] are approximately static; directly scales the ALP fluence and therefore the SK bound.
  • Progenitor mass for SN profiles = 18 solar masses
    Section III; all galactic SNe are modeled with one 18 M_sun AGILE-BOLTZTRAN profile. The authors note lower-mass progenitors have ~20% lower temperatures and densities, but this spread is not propagated into the bound.
  • ALP-nucleon couplings Cap, Can = Cap=-0.47, Can=0
    Chosen in Section III in analogy with the KSVZ model; the excluded region is presented for this benchmark, and changing the coupling ratio would shift the constraint.
assumptions (5)
  • domain assumption Proto-NS temperature and density profiles are unchanged by massive ALP emission.
    Stated in Section III: 'in Ref. [24], it was shown that for massless ALPs the SN profiles are not affected. For simplicity, we assume that this is also the case for our massive ALPs.' If trapped ALPs transport energy, the emission spectrum changes.
  • domain assumption All galactic core-collapse SNe share the same 18 solar-mass AGILE-BOLTZTRAN profile and 0.5-2 s emission window.
    Section III: 'we have assumed that the profiles of all galactic SNe are equivalent to that of a core-collapse SN from an 18 M_sun progenitor.' The paper acknowledges up to 20% lower T and rho for lower-mass progenitors but does not include the spread.
  • domain assumption ALPs are long-lived enough to cross the galaxy, with decay length >= d_g.
    Section III: 'the diffuse galactic flux is only possible for long-lived ALPs... This is possible in some general high-energy ALP theories...' This restricts the models covered by the bound.
  • domain assumption The galactic supernova rate and spatial distribution are given by the exponential disk model of Ref. [50] with 1.63 events per century.
    Used in Eq. (10)-(12); normalization A = 6.40e-4 kpc^-3 yr^-1 is taken from measured rates with ~30% uncertainty, not fit to the ALP signal.
  • standard math Wilks' theorem applies to the binned Poisson likelihood to set 95% C.L. thresholds.
    Appendix B uses chi-square thresholds with dof = bins - 2; asymptotic approximation, acceptable given bin counts but not exact for low-count bins.

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Pith. "Pith review of Probing a diffuse flux of axion-like particles from galactic supernovae with neutrino water Cherenkov detectors." pith.science (2026). https://pith.science/paper/UT3WGV46

@misc{pith2026241209595,
  author       = {Pith},
  title        = {Pith review of: Probing a diffuse flux of axion-like particles from galactic supernovae with neutrino water Cherenkov detectors},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/UT3WGV46}},
  note         = {Machine review of arXiv:2412.09595}
}
abstract

In this article, we claim that axion-like particles (ALPs) with MeV masses can be produced with semi-relativistic velocities in core-collapse supernovae (SNe), generating a diffuse galactic flux. We show that these ALPs can be detected in neutrino water Cherenkov detectors via $a \, p \rightarrow p \, \gamma$ interactions. Using Super-Kamiokande data, we derive new constraints on the ALP parameter space, excluding a region spanning one order of magnitude in the ALP-proton coupling above cooling bounds for ALP masses in the range of $1-70$~MeV and ALP-proton couplings between $\sim 2\times10^{-5}-2\times10^{-4}$. We show that the future Hyper-Kamiokande will be able to probe couplings as small as $\sim 10^{-5}$, considerably constraining the allowed region above SN 1987A cooling bounds.

Figures

Figures reproduced from arXiv: 2412.09595 by the authors.

Figure 1
Figure 1. FIG. 1: ALP flux from galactic SNe that reaches Earth as a function of the ALP energy. In the [PITH_FULL_IMAGE:figures/full_fig_p007_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2: Feynman diagrams of the detection process. [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3: Expected event rate in Super-Kamiokande phase IV via [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: FIG. 4: Bounds on the ALP parameter space, ALP-proton coupling constant vs ALP mass. The [PITH_FULL_IMAGE:figures/full_fig_p010_4.png]
Figure 5
Figure 5. Figure 5: FIG. 5: ALP production spectrum (left panel) and mean free path (right panel) from nucleon [PITH_FULL_IMAGE:figures/full_fig_p014_5.png]
Figure 6
Figure 6. Figure 6: FIG. 6: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p015_6.png]

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 3 Pith papers

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

  1. MeV Electrophilic Axion-like Particles from Sun

    hep-ph 2026-07 conditional novelty 6.0 of 10

    MeV axion-like particles could be made when 5.5 MeV solar fusion photons Compton-scatter off electrons; current LZ, PandaX-4T and Borexino data would then constrain g_ae to (1.7-3.7)e-6 in the 0.4-1 MeV window.

  2. Disentangling axion-like particle couplings to nucleons via a delayed signal in Super-Kamiokande from a future supernova

    hep-ph 2024-12 conditional novelty 6.0 of 10

    A future nearby supernova could reveal sub-MeV axion-like particles through a delayed ~30 MeV photon signal in Super-Kamiokande and Hyper-Kamiokande, probing couplings down to about 3 x 10^-6.

  3. Fresh look at the diffuse ALP background from supernovae

    hep-ph 2025-05 conditional novelty 4.0 of 10

    Adding pion conversion to the diffuse supernova ALP background tightens the Fermi-LAT bound on the ALP-photon coupling to about 2e-13 GeV^-1 for ultralight ALPs, and SN 1987A remains roughly ten times stronger.

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