Ice Cube Observed PeV Neutrinos from AGN Cores

Floyd W. Stecker

REVIEW

Ice Cube Observed PeV Neutrinos from AGN Cores

Floyd W. Stecker

High Energy Astrophysical Phenomena · Submitted 31 May 2013 · 10 references

Pith's verdict: A genuine pre-data prediction of a PeV-peaked AGN-core flux, but 'explains' outruns a ~6-vs-2 event comparison the paper never tests statistically.

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arXiv ID1305.7404 (version 2)

Pith ID6BJOB66O, Pith's permanent record of this paper and its review

CitationFloyd W. Stecker. "Ice Cube Observed PeV Neutrinos from AGN Cores." arXiv:1305.7404 (2013). https://pith.science/paper/6BJOB66O

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Editor's note

read the letter

Stecker is cashing in an old chip, and it's a real one. The AGN-core neutrino flux was fixed in 2005, eight years before IceCube's PeV events, and it predicted a peak at ~1 PeV with isotropic arrival. That timing is the paper's whole value, and it's not nothing: this is a prediction test, not a fit. The Glashow-resonance point is also correct and easy to miss — the π+ → μ+ → e+ chain gives more ν_e than ν̄_e, which suppresses the 6.3 PeV resonance. Nice detail for a two-page letter. The arithmetic also checks out once you do it: E²Φ ≈ 5.6×10⁻⁸ GeV cm⁻² s⁻¹ sr⁻¹ at 1 PeV, 5 m² effective area, 615.9 days, 4π sr gives ~2 events per flavor, ~6 for three. The paper doesn't show that sum, which is annoying but not wrong. Where it overreaches is the words 'explains' and 'significant.' Six predicted against two observed at PeV is P(N≤2|6) ≈ 6% — a mild deficit, not a confirmation. No Poisson or likelihood comparison is made. The factor-20 rescaling from 2005 is the entire basis for the agreement, and the paper names AGN number density as the dominant uncertainty without giving a value or range; a factor of three either way spans the whole observed sample. The honest statement is 'consistent with,' not 'explains.' The 'no conflict' with the extragalactic gamma-ray and UHECR backgrounds is one qualitative sentence plus a citation to Roulet et al.; the reprocessed cascade spectrum is not computed or compared to the measured EGB. That's the weakest section. One thing to fix: the spectral index statements contradict each other. 'E^-2.1 between 1 and 10 PeV' and 'average slope ~3.1 between 1 and 100 PeV' can't both be right, and 3.1 is also inconsistent with the E^-2 shock spectrum invoked two sentences earlier. Probably a typo, but as written it's a real inconsistency. Who should read it: anyone working on IceCube source models or AGN-core neutrino production. Treat it as a checkable claim, not a settled result. Peer review: yes, send it out. The pre-data timing earns a referee's time, but the referee should demand the event-rate formula, a Poisson comparison, and a fix to the spectral index.

Referee report

Significance

The genuine strength here is timing: the spectral shape and the ~1 PeV peak were fixed in 1991 and revised in 2005, well before the 2013 IceCube data, so this is a real prediction test rather than a post-hoc fit, and the paper correctly notes that isotropy is an automatic consequence of an extragalactic source population. If the normalization and the background argument hold up, the result would be a meaningful point in favor of hadronic AGN cores as the PeV neutrino source. The claim is falsifiable in the near term by more IceCube exposure, which is a virtue. However, the confrontation is at the factor-of-a-few level, which is the same order as the theoretical and observational uncertainties the paper itself acknowledges, so the manuscript as written supports 'consistent with' more strongly than 'explains'.

Major objections (5)

[Event-rate paragraph ('Given the effective area of Ice Cube ... ~6 neutrino induced events')] The ~6-event estimate cannot be reproduced from the numbers given in the manuscript. The quoted 'total predicted nu flux at ~1 PeV of ~6e-14 (cm^2 s sr)^-1' has no energy^-1 in its units, so it is unclear whether it is a differential flux at 1 PeV or a band-integrated flux; taking it as the differential value implied by E^2 Phi = 5.6e-8 GeV cm^-2 s^-1 sr^-1 at 1 PeV, and folding with 4 pi, 5 m^2 and 615.9 days, gives of order 2 events per flavor over a decade of bandwidth, not 6. Reaching 6 appears to require either a three-flavor sum or a wider bandwidth, and neither is stated. The paragraph should give the explicit integral N = 4 pi T integral dE Phi(E) A_eff(E), state the assumed energy band and the flavor content of Phi, and show the arithmetic. As written, the central quantitative step of the paper is not checkable.
[Paragraph beginning 'The new estimate was obtained by lowering the flux ... by a factor of 20'] The factor-of-20 rescaling inherited from Ref. [5] is the entire basis for the claimed agreement, and its uncertainty is neither given nor propagated. The manuscript itself identifies the AGN number density per Mpc^3 as the dominant uncertainty but supplies no value or range; a factor of three in either direction moves the predicted count from ~6 to ~2 or ~18, which spans the observed sample. Because the agreement is claimed at exactly this factor-of-a-few level, the paper should either quote a plausible range for the AGN density and show the resulting spread in expected events, or explicitly downgrade the claim from 'explain' to 'consistent with' in the abstract and conclusion.
[Event-rate paragraph and conclusion] No statistical comparison is made between the predicted rate and the observed one. The paper calls the agreement 'significant' without stating how many events are being compared, over what energy band, or what Poisson probability attaches to the comparison; a prediction of 6 against 2 observed at ~1 PeV corresponds to P(N <= 2 | 6) of order 6%, which is a mild deficit rather than a confirmation. A short Poisson statement, with the observed count and band defined, is needed before the word 'significant' can carry the weight the abstract places on it.
[Abstract and paragraph beginning 'Since the secondary gamma-rays from Delta+ -> p + pi0 ...'] The clause 'without conflicting with the constraints from the observed extragalactic cosmic ray and gamma-ray backgrounds' is load-bearing for the abstract's claim but is supported only by the qualitative statement that secondary gamma rays and protons lose energy in the source, plus a citation to Ref. [9]. The reprocessed cascade spectrum that would actually be compared to the measured extragalactic gamma-ray background is not computed or shown, and it is not made explicit which result in Ref. [9] supplies the bound and under what assumptions it applies to this model. Either a short cascade estimate with the resulting gamma-ray flux compared to the measured background should be included, or the sentence should be rephrased to state that the background consistency is argued qualitatively and refer the reader to the specific section of Ref. [9] that establishes it.
[Paragraph beginning 'The main uncertainty in the magnitude of the modeled flux ...'] There is an internal inconsistency in the stated spectral shape. The text says the neutrino spectrum 'was predicted to be proportional to E^-2.1 between 1 and 10 PeV' and then, two sentences later, that 'the average slope of the neutrino spectrum was predicted to be ~3.1 between 1 and 100 PeV'. These two ranges overlap and the indices differ by one unit; unless a spectral break is intended, one of the numbers is wrong. Since the spectral index is one of the few pre-data predictions the paper is testing, this should be corrected and, if a break is intended, its energy should be stated.

Minor objections (7)

[Title and throughout] The collaboration and detector name is styled 'IceCube' in the literature; the manuscript uses 'Ice Cube' throughout, including the title.
[First paragraph] The phrase 'the first observation of cosmic 2 PeV energy neutrinos' is ambiguous between 'two PeV-energy neutrinos' and 'neutrinos of 2 PeV'; the sentence should be reworded to make the event count and energies explicit.
[First paragraph] The figure of 18 events at ~4 sigma above atmospheric background above 100 TeV is attributed to Ref. [2], a conference proceedings, rather than to the IceCube publication Ref. [1]; the number should be cross-checked against, and cited to, the published source where possible.
[Event-rate paragraph] The calculation uses the IceCube effective area 'for an isotropic flux of nu_e's at ~1 PeV of 5 m^2' together with a flux normalization quoted for nu_mu. The flavor mismatch should be resolved, and the effective area at the relevant energies for the relevant channel stated explicitly.
[Paragraph on Glashow resonance] The statement that 'there will be both more and higher energy nu_e's produced than anti-nu_e's' is only half right: the nu_e from muon decay carries roughly a quarter of the pion energy, the same fraction as the other leptons, so the 'higher energy' qualifier is not supported by the decay chain as described. The argument that the nu_e excess suppresses the 6.3 PeV Glashow resonance is sound and should be kept, but the energy claim should be removed or justified.
[Throughout] The paper would be considerably easier to assess with a single figure showing E^2 Phi versus E for the model prediction together with the IceCube event energies, and with the relevant curve from Ref. [4] reproduced or at least digitized so the factor-of-20 rescaling can be checked by eye.
[Paragraph beginning 'The new estimate was obtained ...'] The sentence 'The peak flux in these units occurs at an energy ~1 PeV' is missing a terminal period.

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The paper

The paper claims

The neutrino flux predicted from the cores of active galaxies, scaled down twentyfold from its 1991 estimate, is enough to account for the PeV neutrinos IceCube has seen, and it peaks at just the energy where they appear.

The reading

IceCube has reported a handful of neutrino events at energies of hundreds of TeV to a few PeV, appearing isotropic on the sky and falling roughly as $E^{-2}$. Stecker argues that a model he and collaborators proposed in 1991 — protons accelerated by shocks near the black hole accretion disk in active galactic nuclei, trapped in the disk's magnetic field, and converted to pions on the dense thermal photon field of the accretion disk — already predicts a neutrino flux with the right peak energy, the right slope, and roughly the right normalization to produce those events. The normalization is the 1991 prediction lowered by a factor of 20 following later observations and the discovery of neutrino oscillations; with that rescaling the model yields of order six neutrino-induced events in the 615.9-day exposure IceCube reported. The claim matters because it would give the first cosmic neutrinos a known source class, and because the same model was built so that its secondary gamma rays are absorbed inside the source and its protons do not reach ultrahigh energies, so it does not overshoot the measured extragalactic gamma-ray or cosmic-ray backgrounds.

What carries the argument

The mechanism is photomeson production by shock-accelerated protons on the dense optical/UV photon field of the AGN accretion disk — the 'big blue bump' — which is optically thick to protons and keeps them from escaping at ultrahigh energies. The $\Delta$-resonance channel near threshold fixes the energy budget: the pion inherits about a fifth of the proton energy, and each of the four leptons in the subsequent decays takes about a quarter of the pion energy. That two-step division is what places the neutrino peak near 1 PeV for protons accelerated to modest energies, and it is what ties the neutrino flux to the same photon field that absorbs the accompanying gamma rays inside the source.

Extended reading notes

Core claim

The paper's claim is that the AGN-core model, as revised in 2005, can explain the IceCube PeV events without violating any existing background constraint. In the model, protons are accelerated in the AGN core and lose energy through photomeson production on the accretion disk's thermal emission, chiefly through the channel $p + gamma -> Delta+ -> n + pi+$; the pion carries roughly 0.2 of the proton energy, and its decays $pi+ -> mu+ + nu_mu$, $mu+ -> anti-nu_mu + nu_e + e+$ distribute that energy among neutrinos. The predicted flux is about $10^{-8}$ GeV cm$^{-2}$ s$^{-1}$ sr$^{-1}$ in $E^2 Phi$ at 100 TeV, rising to about $5.6 imes 10^{-8}$ at 1 PeV, with the peak in these units near 1 PeV, and a total neutrino flux at 1 PeV of about $6 imes 10^{-14}$ (cm$^2$ s sr)$^{-1}$. Combining that with IceCube's effective area for an isotropic electron-neutrino flux at 1 PeV of about 5 m$^2$ and 615.9 days of exposure, the paper predicts roughly six neutrino-induced events — the same order as the reported sample. Because the decay chain produces more electron neutrinos than antineutrinos, the Glashow resonance at 6.3 PeV is suppressed in the detector, another check the author notes. The predicted spectrum is $E^{-2.1}$ between 1 and 10 PeV for a proton spectrum of $E^{-2}$, and the sources being extragalactic, the arrival directions should be roughly isotropic.

Load-bearing premise

The argument rests on taking the factor-of-20 downward rescaling of the 1991 flux as the correct normalization; the paper itself names the AGN number density per cubic megaparsec as the dominant uncertainty but gives no value or range for it, and a factor-of-three change either way would move the predicted count from about six to about two or about eighteen.

Editorial extensions

If this is right

IceCube's event rate above 100 TeV should continue at roughly the level the model predicts, about six events per 616 days of exposure for an isotropic flux.
The neutrino energy spectrum should peak in $E^2 Phi$ near 1 PeV and steepen above it, rather than continue as a single unbroken power law to higher energies.
The arrival directions should be isotropic, with no strong correlation to the nearest individual AGN, since the sources are extragalactic and numerous.
A suppressed Glashow resonance at 6.3 PeV is expected because the decay chain yields more electron neutrinos than antineutrinos.
The accompanying gamma rays should be absorbed inside the source by pair production, so the model adds no detectable bump to the extragalactic gamma-ray background.
Protons in this model should not reach ultrahigh energies, so the observed ultrahigh-energy cosmic-ray flux must come from elsewhere.

Reading between the lines

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

If the AGN-core normalization is really fixed by the number density of AGN per cubic megaparsec, then a future census of local Seyferts and their accretion-disk photon fields could turn this from a fit into a prediction, since the paper leaves that density unquantified.
The predicted isotropy and the absence of bright individual sources make a stacking search on nearby Seyfert galaxies the natural next test: a null result there would not kill the model, but a positive correlation would be hard to attribute to anything else.
The same proton-loaded, photon-thick core that suppresses the gamma-ray background should also be a source of neutrinos from heavier nuclei if the accelerated population is not pure hydrogen, which would shift the peak energy and is not considered here.
Because the model's neutrino peak sits at the energy where IceCube's effective area is small, the next generation of larger detectors should see the peak sharpen into a spectral feature rather than a single power law, which is a cleaner discriminator than the total rate.

Original abstract

I show that the high energy neutrino flux predicted to arise from AGN cores can explain the PeV neutrinos detected by Ice Cube without conflicting with the constraints from the observed extragalactic cosmic ray and gamma-ray backgrounds.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.12 · human participants 0.02 · controlled comparison 0.06 · randomized assignment 0.01 · states quantitative result 0.06 · compares with prior results 0.46 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; show every role.

I show that the high energy neutrino flux predicted to arise from AGN cores can explain the PeV neutrinos detected by Ice Cube without conflicting with the constraints from the observed extragalactic cosmic ray and gamma-ray backgrounds.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	I show that the high energy neutrino flux predicted to arise from AGN cores can explain the PeV neutrinos detected by Ice Cube without conflicting with the constraints from the observed extragalactic cosmic ray and gamma-ray backgrounds.	result 0.78	0.78	0.93	asserted 1.00

What kind of paper the classifier reports this is: theoretical result 0.96 · evidence from argument 0.61.

What was examined, and what was not

sources read

arXiv listing abstract v2

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

References

Works cited (10)

[5]

F. W. Stecker, Phys. Rev. D 72, 107301 (2005)

View on Pith 2005
[9]

E. Roulet et al., J. Cosmol. Astropart. Phys. 2013/01/02 8 (2013)

View on Pith 2013
[1]

M. G. Aartsen et al., arXiv:1304.5356

View on Pith Pith review arXiv
[2]

F. Halzen, Proc. 33rd Intl. Cosmic Ray Conf., Rio de Janiero, 2013. 2

View on Pith 2013
[3]

F. W. Stecker, C. Done, M.H. Salamon and P. Sommers, Phys. Rev. Lett. 66, 2697 (1991),

View on Pith 1991
[4]

F. W. Stecker, Phys. Rev. Lett. 69, 2738 (1992)

View on Pith 1992
[6]

D. Kazanas and D. C. Ellison, Astrophys. J. 304, 178 (1986)

View on Pith 1986
[7]

A. Laor, Mon. Not. Royal Astr. Soc. 246, 369 (1990)

View on Pith 1990
[8]

F. W. Stecker, Phys. Rev. Lett. 21, 1016 (1968)

View on Pith 1968
[10]

S. L. Glashow, Phys. Rev. 118, 316 (1960)

View on Pith 1960

Forward citations

Cited by 23 Pith papers

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

Hidden Cores of Active Galactic Nuclei as the Origin of Medium-Energy Neutrinos: Critical Tests with the MeV Gamma-Ray Connection
astro-ph.HE 2019-04 conditional novelty 6.0 of 10

Stochastic proton acceleration in AGN coronae, with cosmic rays at about one percent of the thermal energy, reproduces the IceCube 10 to 100 TeV neutrino flux and predicts a correlated MeV gamma-ray background.
Imaging Galactic Dark Matter with High-Energy Cosmic Neutrinos
hep-ph 2017-03 conditional novelty 6.0 of 10

Scattering between cosmic neutrinos and Galactic dark matter would suppress the flux from the Galactic center; IceCube's four-year event sample constrains this coupling in a region of parameter space beyond cosmologic...
Hidden Cosmic-Ray Accelerators as an Origin of TeV-PeV Cosmic Neutrinos
astro-ph.HE 2015-09 conditional novelty 6.0 of 10

The TeV-PeV IceCube neutrino flux implies that its sources are opaque to GeV gamma rays, so the accelerators are hidden from Fermi and should be sought in X-rays and MeV gamma rays.
Spectral analysis of the high-energy IceCube neutrinos
astro-ph.HE 2015-02 conditional novelty 6.0 of 10

Joint spectral and flavor fits to 36 IceCube events show the inferred neutrino flavor mix and spectral index depend strongly on the chosen energy window, with a 10 PeV cutoff favoring tau dominance.
Atmospheric and Astrophysical Neutrinos above 1 TeV Interacting in IceCube
astro-ph.HE 2014-10 accept novelty 6.0 of 10

A veto-based IceCube search extends the astrophysical neutrino measurement down to 10 TeV and yields a spectral index of 2.46 ± 0.12, softer than the E^-2 benchmark, plus a prompt-atmospheric limit of 1.52 times the b...

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A light scalar that mediates lepton-number violation generates Majorana neutrino masses and, at the same time, a neutrino self-interaction whose resonant absorption feature IceCube could detect in about ten years.
The Direct Detection of Boosted Dark Matter at High Energies and PeV events at IceCube
hep-ph 2014-07 conditional novelty 6.0 of 10

A boosted dark matter component scattering neutral-current-like off nucleons can reproduce the three PeV IceCube cascades using a 5 PeV parent relic, a 10 GeV dark fermion, and a 5 TeV Z-prime mediator.
Reconstruction of Interstellar Cosmic Ray Anisotropy via Heliospheric Propagation Modeling and SVD Inversion
astro-ph.HE 2026-10 conditional novelty 5.0 of 10

A heliospheric transport simulation plus SVD inversion recovers the interstellar cosmic-ray dipole once a circle-fitting algorithm restores the detector-blind North-South component, with Poisson count noise dominating...
Constraining High-Energy Cosmic Neutrino Sources: Implications and Prospects
astro-ph.HE 2016-07 accept novelty 5.0 of 10

Non-detection of multiple high-energy muon tracks from any sky direction implies a lower bound on the local density of steady neutrino sources, which rules out rare bright blazars as the dominant source class.
Analysis of the 4-year IceCube high-energy starting events
astro-ph.HE 2016-05 conditional novelty 5.0 of 10

Using 53 public IceCube high-energy starting events, the authors find a softer astrophysical neutrino spectrum than IceCube's preliminary fit, no significant preference for two power laws, and no North-South asymmetry...
Probing BSM Neutrino Physics with Flavor and Spectral Distortions: Prospects for Future High-Energy Neutrino Telescopes
astro-ph.HE 2015-12 conditional novelty 5.0 of 10

A forecast shows that IceCube-Gen2, using Glashow resonance and double-bang events alongside showers and tracks, could constrain or discover neutrino decay, pseudo-Dirac states, and secret neutrino self-interactions.
Testing the Dark Matter Scenario for PeV Neutrinos Observed in IceCube
hep-ph 2015-03 conditional novelty 5.0 of 10

Very heavy decaying dark matter stays marginally consistent with the Fermi diffuse gamma-ray background, and the scenario can be settled by sub-PeV gamma-ray data or by IceCube-Gen2 muon searches toward Virgo.
Possible Interpretations of IceCube High-Energy Neutrino Events
hep-ph 2014-11 conditional novelty 5.0 of 10

Three different explanations of the IceCube 37-event sample (power law, power law plus PeV particle decay, decay only) all fit the energy spectrum comparably, and the paper projects the exposure needed to separate them.
C\nu B absorption line in the neutrino spectrum at IceCube
hep-ph 2014-07 conditional novelty 5.0 of 10

The 500 TeV to 1 PeV gap in the IceCube neutrino spectrum can be fit as resonant absorption on the cosmic neutrino background via a new scalar of roughly 3 MeV, given a neutrino mass near 5.6 meV.
Star-forming galaxies as the origin of diffuse high-energy backgrounds: Gamma-ray and neutrino connections, and implications for starburst history
astro-ph.HE 2014-04 conditional novelty 5.0 of 10

Starburst galaxies with cosmic-ray spectral index near 2.15 can jointly reproduce the Fermi diffuse gamma-ray background and a large fraction of the IceCube PeV neutrino flux.
Probing the Galactic Origin of the IceCube Excess with Gamma-Rays
astro-ph.HE 2013-09 conditional novelty 5.0 of 10

Existing TeV to PeV diffuse gamma-ray limits disfavor an isotropic Galactic origin for the IceCube neutrino excess, supporting a mostly extragalactic interpretation, though the relevant Southern Sky is poorly covered.
Demystifying the PeV Cascades in IceCube: Less (Energy) is More (Events)
astro-ph.HE 2013-06 conditional novelty 5.0 of 10

Two PeV cascade events in IceCube are inconsistent with atmospheric conventional and cosmogenic neutrino fluxes, and dedicated sub-PeV cascade searches would identify the true source fastest.
Searching for MeV-Scale Gauge Bosons with IceCube
hep-ph 2015-07 conditional novelty 4.0 of 10

A light Z' coupling to neutrinos would carve an absorption dip in the IceCube spectrum, and existing data already rule out the lightest such particles in the inverted-hierarchy scenario.
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astro-ph.HE 2014-12 conditional novelty 4.0 of 10

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Geometric Compatibility of IceCube TeV-PeV Neutrino Excess and its Galactic Dark Matter Origin
hep-ph 2013-11 conditional novelty 4.0 of 10

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astro-ph.HE 2013-12 conditional novelty 3.0 of 10

The 28 IceCube neutrino events are consistent with either Galactic or extragalactic sources, and a single power law of index 2.3 fits the spectrum without requiring a cutoff above 2 PeV.
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How the literature uses it

43 arXiv papers cite this in 49 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers whose main result relates to this one's

Found among the papers closest to this one by title and main claim. Pith's classifier compared each pair's main results and a second model family confirmed the relation; checked against two further families, shown conflicts agreed 118 times in 120 and shown same results 218 times in 239. The quoted sentence is the other paper's main claim.

States the same result 1 paper

We show that this model can explain detected neutrino flux and avoids, at the same time, existing constraints from the gamma-ray and cosmic ray observations.

Neutrinos in IceCube from AGN's · 1.00

Papers citing it · 23 sentences without a confident label

Cites it as support 2 papers

AGN core models may explain the IceCube data [ref] , and such hidden CR accelerators are suggested by the latest IceCube data [ref] .

Active Galactic Nuclei as High-Energy Neutrino Sources · AGN Cores · 0.99
These include GRBs [ref] , AGNs [ref] , and hypernova remnants in star forming galaxies [ref] .

Cosmic Neutrino Pevatrons: A Brand New Pathway to Astronomy, Astrophysics, and Particle Physics · Looking Ahead · 0.96

Cites it as background 24 papers

The observation can be most probably associated with various extragalactic $∼100$ PeV cosmic-ray accelerators, e.g. low-power gamma-ray burst jets [ref] , AGN [ref] , star-forming galaxies including starbursts, galaxy mergers and AGN [ref] , intergalactic shocks and active galaxies embedded in structured regions [ref] .

Star-forming galaxies as the origin of diffuse high-energy backgrounds: Gamma-ray and neutrino connections, and implications for starburst history · Introduction · 0.82
Among the possibilities explored are viable astrophysical sources [ref] , a possible DM connection [ref] , a leptoquark resonance [ref] , the decay of massive neutrinos [ref] , the decay of a very heavy long-lived particle [ref] or even the possibility that these events could be understood in terms of novel interactions that neutrinos have with the cosmic neutrino background [ref] .

Possible Interpretations of IceCube High-Energy Neutrino Events · Introduction · 0.93
In the literature, the suggested sources for PeV neutrinos include active galactic neucleis (AGNs, [ref] ), star forming galaxies (SFGs, [ref] ), clusters of galaxies [ref] , hypernovae (HNe, [ref] ), gamma-ray bursts (GRBs, see [ref] , but see [ref] ), and cosmogenic neutrinos (see [ref] , but see [ref] ).

TeV-PeV neutrinos over the atmospheric background: originating from two groups of sources? · Introduction · 0.99

What it cites · 1 sentence without a confident label

Uses data or values from 1 paper

Given the effective area of Ice Cube for an isotropic flux of $ν_e$'s at $∼$1 PeV of 5 m$^2$ and an exposure time of 615.9 days [ref] , and giving a total predicted $ν$ flux at $∼$1 PeV of $∼6 ×10^-14$ (cm$^2$ s sr)$^-1$, we would predict that Ice Cube should see a total of $∼$6 neutrino induced events.

First observation of PeV-energy neutrinos with IceCube · Introduction · 1.00

Discussion

Disagree with the review, or know something it missed? Leave a comment, highlight any passage above to comment on it, or challenge this review formally.

[1] [5]

F. W. Stecker, Phys. Rev. D 72, 107301 (2005)

View on Pith 2005

[2] [9]

E. Roulet et al., J. Cosmol. Astropart. Phys. 2013/01/02 8 (2013)

View on Pith 2013

[3] [1]

M. G. Aartsen et al., arXiv:1304.5356

View on Pith Pith review arXiv

[4] [2]

F. Halzen, Proc. 33rd Intl. Cosmic Ray Conf., Rio de Janiero, 2013. 2

View on Pith 2013

[5] [3]

F. W. Stecker, C. Done, M.H. Salamon and P. Sommers, Phys. Rev. Lett. 66, 2697 (1991),

View on Pith 1991

[6] [4]

F. W. Stecker, Phys. Rev. Lett. 69, 2738 (1992)

View on Pith 1992

[7] [6]

D. Kazanas and D. C. Ellison, Astrophys. J. 304, 178 (1986)

View on Pith 1986

[8] [7]

A. Laor, Mon. Not. Royal Astr. Soc. 246, 369 (1990)

View on Pith 1990

[9] [8]

F. W. Stecker, Phys. Rev. Lett. 21, 1016 (1968)

View on Pith 1968

[10] [10]

S. L. Glashow, Phys. Rev. 118, 316 (1960)

View on Pith 1960