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arxiv: 2404.15944 · v2 · submitted 2024-04-24 · 🌌 astro-ph.HE

IceCube Results and Perspective for Neutrinos from LHAASO Sources

Ke Fang , Francis Halzen This is my paper

Pith reviewed 2026-05-24 01:47 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords IceCube neutrinosGalactic planeLHAASO sourcesPeVatronsmultimessenger astronomycosmic-ray interactionsGRB 221009A
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The pith

IceCube data show neutrinos from the Galaxy do not dominate the neutrino sky, unlike the Milky Way's role at every other wavelength.

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

The paper reviews ten years of IceCube results on cosmic neutrinos and stresses multimessenger observations as the route to confirming neutrinos from the Milky Way itself. It calculates the neutrino output expected when Galactic cosmic rays collide with interstellar gas and finds this component remains a minor part of the total neutrino sky. The contrast with radio, optical, and gamma-ray skies, where the Galaxy is bright and structured, is presented as a central observation. The authors then examine how neutrino and gamma-ray data together can test whether LHAASO sources are hadronic PeVatrons and review the search for neutrinos from the bright transient GRB 221009A.

Core claim

The neutrino flux generated by Galactic cosmic rays interacting with the interstellar medium does not form a dominant or structured feature in the high-energy neutrino sky, in contrast to the prominent Galactic emission seen in every other wavelength band.

What carries the argument

Standard modeling of Galactic-plane neutrino production from cosmic-ray propagation and pp interactions, compared directly with LHAASO gamma-ray maps to identify hadronic sources.

If this is right

  • Joint neutrino and gamma-ray maps can isolate the fraction of LHAASO sources whose emission is hadronic rather than purely electromagnetic.
  • Absence of a strong Galactic neutrino signal implies that most observed neutrinos arrive from extragalactic accelerators.
  • Targeted neutrino searches around individual LHAASO sources and transients such as GRB 221009A become the practical route to identifying PeVatrons.
  • Future analyses can use the same modeling framework to set upper limits on any additional Galactic neutrino component beyond the standard interstellar-medium prediction.

Where Pith is reading between the lines

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

  • If the Galactic neutrino contribution stays small, the diffuse neutrino background is likely produced by a population of distant sources whose collective output exceeds local cosmic-ray interactions.
  • This pattern suggests that cosmic-ray confinement or interaction efficiency inside the Milky Way differs from the assumptions that work well for gamma rays.
  • Dedicated point-source searches with next-generation detectors may yield faster progress than all-sky diffuse analyses focused on the plane.

Load-bearing premise

The neutrino output from the Galactic plane can be calculated accurately from conventional models of cosmic-ray transport and their collision rates with interstellar gas.

What would settle it

An observation of a bright, plane-like neutrino excess whose intensity and morphology make the Galaxy the brightest feature in the neutrino sky rather than a subdominant component.

Figures

Figures reproduced from arXiv: 2404.15944 by Francis Halzen, Ke Fang.

Figure 1
Figure 1. Figure 1: Flow diagram showing the production of charged and neutral pions in pγ interactions. The circles indicate equal energy going into gamma rays and into pairs of muon neutrinos and antineutrinos, which IceCube cannot distinguish between. Because the charged pion energy is shared roughly equally among four particles and the neutral pion energy among two photons, the photons have twice the energy of the neutrin… view at source ↗
Figure 2
Figure 2. Figure 2: Energy spectra of secondary gamma rays (red) and neutrinos (blue) from the interaction between proton (dark colors)/helium (light colors) primaries and rest-mass proton targets. The primary spectrum in use is dN/dE = E−2 exp(−E/10PeV), with E = Ep = EHe/4 being the energy per nucleon. We have set Emin = 2.5 GeV. The secondary spectra are computed using the aafragpy package [12] with cross sections from [13… view at source ↗
Figure 3
Figure 3. Figure 3: Current all-sky measurements of the high-energy astrophysical neutrino emission. The flux of cosmic muon neutrinos [16] inferred from the 9.5-year upgoing-muon track analysis (solid line) with 1σ uncertainty range (shaded) is compared with the flux of showers initiated by electron and tau neutrinos [18], when assuming standard oscillations. The measurements are consistent with the expectation that each neu… view at source ↗
Figure 4
Figure 4. Figure 4 [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The plane of the Milky Way galaxy in photons and neutrinos. Each panel from top to bottom shows the flux in latitude and longitude: (A) Optical flux. (B) The integrated flux in gamma rays from the Fermi-LAT 12-year survey at energies greater than 1 GeV. (C) The neutrino emission template derived from the π 0 template that matches the Fermi-LAT observations of the diffuse gamma-ray emission. (D) The emissio… view at source ↗
Figure 6
Figure 6. Figure 6: The energy spectra of neutrinos from the Galactic plane measured using three templates of the diffuse neutrino emission: the π 0 , KRA5 γ and KRA50 γ models (from [5]). Dotted curves indicate the model flux while solid curves and shaded regions indicate the measured flux and 1σ uncertainties, respectively. The hatched region shows the IceCube all-sky diffuse flux [48]. at the same time that given the uncer… view at source ↗
Figure 7
Figure 7. Figure 7: The neutrino flux of the Galactic plane. The neutrino flux is shown in blue with a spread that includes statistical and systematic errors. The accompanying gamma-ray flux shown in red matches the lower energy Fermi data. Both are consistent with a model (dashed lines) determining the number of parent pions produced in interactions of Galactic cosmic rays interacting with the interstellar medium. The neutri… view at source ↗
Figure 8
Figure 8. Figure 8: Cosmic-ray proton (top curve) and helium (bottom curve) fluxes at the Earth between 1 GeV and 108 GeV scaled by E2.7 (adapted from Ref. [6]). The data points are from measurements by AMS-02 [67, 68], PAMELA [69], ATIC [70], CALET [71, 72], CREAM-III [73], DAMPE [74], NUCLEON [75], KASCADE [76], and IceTop [77] experiments. The errors indicate the quadratic sums of statistical and systematic uncertainties o… view at source ↗
Figure 9
Figure 9. Figure 9: Intensities of Galactic diffuse emission in gamma rays and neutrinos from two sky regions, region A (left): 25◦ < l < 100◦ , |b| < 5 ◦ , and region B (right): 50◦ < l < 200◦ , |b| < 5 ◦ (from [6]). The data points refer to observations of various gamma-ray experiments, including Tibet ASγ [53] (orange data points; the fainter data points at 500 TeV indicate the residual intensity after removing events near… view at source ↗
Figure 10
Figure 10. Figure 10: Spectral energy distribution of the gamma-ray emission at the Cocoon region. The data points are from measurements by Fermi-LAT [111, 141], ARGO [142], HAWC [115], and LHAASO [118]. See Section 5 for more discussion regarding the gamma-ray observations of the Cygnus Cocoon. The solid and dashed curves denote two theory models from [115], which invoke continuous proton injection and a recent burst by a PeV… view at source ↗
read the original abstract

We briefly review the main results of the IceCube Neutrino Observatory one decade after the discovery of cosmic neutrinos. We emphasize the importance of multimessenger observations, most prominently for the discovery of neutrinos from our own Galaxy. We model the flux from the Galactic plane produced by Galactic cosmic rays interacting with the interstellar medium and discuss the perspectives of understanding the TeV-PeV emission of the Galactic plane by combining neutrino and gamma-ray observations. We draw attention to the interesting fact that the neutrino flux from the Galaxy is not a dominant feature of the neutrino sky, unlike the case in any other wavelength of light. Finally, we review the attempts to identify PeVatrons by confronting the neutrino and gamma-ray emission of Galactic sources, including those observed by LHAASO. We end with a discussion of searches for neutrinos from LHAASO's extragalactic transient source gamma-ray burst 221009A.

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

1 major / 1 minor

Summary. This review summarizes IceCube's key results on cosmic neutrinos a decade after their discovery, stressing multimessenger observations that enabled the detection of Galactic neutrinos. It presents a model for the neutrino flux from the Galactic plane arising from cosmic-ray interactions with the interstellar medium, notes that this component is sub-dominant in the neutrino sky (unlike in other wavelengths), and discusses prospects for identifying PeVatrons via combined neutrino and LHAASO gamma-ray data on Galactic sources as well as searches for neutrinos from the extragalactic transient GRB 221009A.

Significance. The review usefully frames the unique character of the neutrino sky, where extragalactic sources dominate, and outlines how IceCube-LHAASO multimessenger analyses can constrain Galactic cosmic-ray sources. Credit is given for grounding the discussion in established IceCube detections and standard hadronic interaction physics without introducing new free parameters or ad-hoc entities.

major comments (1)
  1. [Modeling section (abstract and associated discussion)] Modeling section (as described in the abstract): the central claim that Galactic neutrinos are not a dominant feature requires the modeled CR-ISM flux to remain << total IceCube diffuse flux from 10 TeV to PeV. The paper invokes standard propagation and cross-section assumptions but provides neither uncertainty bands on this flux nor an explicit comparison to additional hadronic neutrino contributions from LHAASO PeVatrons (via the same pp interactions producing their gamma rays). This omission is load-bearing because energy-dependent leakage or source grammage not captured in the baseline model could raise the total Galactic fraction enough to challenge the sub-dominance statement.
minor comments (1)
  1. [Abstract] The abstract states that the Galactic neutrino flux 'is not a dominant feature' but does not cite the specific IceCube diffuse flux measurement or energy range used for the comparison, reducing clarity for readers unfamiliar with the referenced data sets.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the constructive feedback. We address the single major comment below.

read point-by-point responses

  1. Referee: [Modeling section (abstract and associated discussion)] Modeling section (as described in the abstract): the central claim that Galactic neutrinos are not a dominant feature requires the modeled CR-ISM flux to remain << total IceCube diffuse flux from 10 TeV to PeV. The paper invokes standard propagation and cross-section assumptions but provides neither uncertainty bands on this flux nor an explicit comparison to additional hadronic neutrino contributions from LHAASO PeVatrons (via the same pp interactions producing their gamma rays). This omission is load-bearing because energy-dependent leakage or source grammage not captured in the baseline model could raise the total Galactic fraction enough to challenge the sub-dominance statement.

    Authors: The modeled CR-ISM neutrino flux is computed from standard propagation parameters (diffusion coefficient, halo height, etc.) calibrated directly to local cosmic-ray measurements and uses the well-measured pp cross section; the resulting flux lies well below the IceCube-measured diffuse spectrum from 10 TeV to PeV, as already shown by multiple prior IceCube analyses. We acknowledge that explicit uncertainty bands are not plotted in the present manuscript. However, the allowed range of propagation parameters is tightly constrained by the cosmic-ray data themselves, and excursions within that range do not bring the Galactic component close to the total observed flux. The LHAASO PeVatrons are treated in a dedicated later section as candidate individual sources; their possible neutrino emission is bounded by the non-observation of neutrinos from those directions, so they do not contribute appreciably to the diffuse flux used in the sub-dominance argument. The baseline model deliberately isolates the truly diffuse ISM component; any additional source grammage would appear as a point-like or extended excess and is already constrained by the same IceCube data. We will revise the modeling section to state these distinctions explicitly and to cite the existing literature bounds on the Galactic neutrino fraction. revision: partial

Circularity Check

0 steps flagged

No circularity: central claims rest on external IceCube/LHAASO observations and standard ISM modeling without self-referential reduction.

full rationale

The paper reviews IceCube results and models Galactic-plane neutrino flux via standard cosmic-ray propagation and pp interaction cross-sections, then compares this to the observed diffuse flux to conclude the Galactic component is sub-dominant. This comparison uses external data and established astrophysical assumptions rather than any fitted parameter redefined as a prediction, self-citation chain, or ansatz smuggled from prior author work. No equations or sections exhibit self-definitional loops or uniqueness theorems imported from the same authors. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The modeling rests on standard domain assumptions about cosmic-ray propagation and neutrino production in the interstellar medium; no free parameters or invented entities are introduced in the abstract.

axioms (1)
  • domain assumption Galactic cosmic rays interact with the interstellar medium to produce neutrinos at TeV-PeV energies
    Invoked when modeling the galactic plane flux.

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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.

  1. Particle Astrophysics with High and Ultrahigh Energy Neutrinos

    astro-ph.HE 2025-11 unverdicted novelty 2.0

    Recent high and ultrahigh energy neutrino detections open a new observational window to the universe by revealing sources and processes inaccessible via photons.

Reference graph

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