Pith. Sign in

REVIEW

Search for Dark Matter WIMPs using Upward Through-going Muons in Super-Kamiokande

PaperPDF from arXiv

data files

ReviewThe objections and verdict, as JSON Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
X Bluesky LinkedIn Reddit Hacker News
Super-Kamiokande Collaboration: S. Desai, Y. Ashie, S. Fukuda, Y. Fukuda, K. Ishihara, Y. Itow, Y. Koshio, A. Minamino
show 127 more authors
M. Miura, S. Moriyama, M. Nakahata, T. Namba, R. Nambu, Y. Obayashi, N. Sakurai, M. Shiozawa, Y. Suzuki, H. Takeuchi, Y. Takeuchi, S. Yamada, M. Ishitsuka, T. Kajita, K. Kaneyuki, S. Nakayama, A. Okada, T. Ooyabu, C. Saji, M. Earl, E. Kearns, J.L. Stone, L.R. Sulak, C.W. Walter, W. Wang, M. Goldhaber, T. Barszczak, D. Casper, J.P. Cravens, W. Gajewski, W.R. Kropp, S. Mine, D.W. Liu, M.B. Smy, H.W. Sobel, C.W. Sterner, M.R. Vagins, K.S. Ganezer, J. Hill, W.E. Keig, J.Y. Kim, I.T. Lim, R.W. Ellsworth, S. Tasaka, G. Guillian, A. Kibayashi, J.G. Learned, S. Matsuno, D. Takemori, M.D. Messier, Y. Hayato, A. K. Ichikawa, T. Ishida, T. Ishii, T. Iwashita, J. Kameda, T. Kobayashi, T. Maruyama, K. Nakamura, K. Nitta, Y. Oyama, M. Sakuda, Y. Totsuka, A.T. Suzuki, M. Hasegawa, K. Hayashi, T. Inagaki, I. Kato, H. Maesaka, T. Morita, T. Nakaya, K. Nishikawa, T. Sasaki, S. Ueda, S. Yamamoto, T.J. Haines, S. Dazeley, S. Hatakeyama, R. Svoboda, E. Blaufuss, J.A. Goodman, G.W. Sullivan, D. Turcan, K. Scholberg, A. Habig, C.K. Jung, T. Kato, K. Kobayashi, M. Malek, C. Mauger, C. McGrew, A. Sarrat, E. Sharkey, C. Yanagisawa, T. Toshito, C. Mitsuda, K. Miyano, T. Shibata, Y. Kajiyama, Y. Nagashima, M. Takita, M. Yoshida, H.I. Kim, H. Okazawa, T. Ishizuka, Y. Choi, H.K. Seo, Y. Gando, T. Hasegawa, K. Inoue, J. Shirai, A. Suzuki, M. Koshiba, T. Hashimoto, Y. Nakajima, K. Nishijima, T. Harada, H. Ishino, M. Morii, R. Nishimura, Y. Watanabe, D. Kielczewska, J. Zalipska, R. Gran, K.K. Shiraishi, K. Washburn, R.J. Wilkes

High Energy Physics - Experiment · Submitted 21 Apr 2004 · 76 references

Pith's verdict: The upward-muon flux limits are solid and worth citing; the abstract's 'model-independent' cross-section limits rest on the Ref. [58] maximum ratio, which the authors' own Sec. V concedes can fail for Higgs/gluon channels.

T0 · AI review

How this review was made: An AI referee (selfhosted/deepseek-v4.1-flash) read the paper on October 29, 2026 and answered a fixed list of questions about it. T0 is the starting level every paper gets. The levels describe how deeply Pith has checked the paper, never the authors.

  1. T0 AI review An AI read the paper and answered a fixed list of questions.
  2. T1 Audit Automatic checks that the references and files the paper relies on exist and match.
  3. T2 Compute The paper's code or calculations re-run with the same results.
  4. T3 Formal statement The claims written out in a formal math language a computer can read.
  5. T4 Proof Those claims proved, and the proof checked by computer.

How Pith checks papers →

· 2 major objections · 9 minor · Ask about this paper · The compiled record · Read the full review →
Challenge this review Comment (0) Read on arXiv ↗
Cite ▾
arXiv IDhep-ex/0404025 (version 2)
Pith IDLQ6YSIO4, Pith's permanent record of this paper and its review
CitationA. Habig, A. Kibayashi, A. K. Ichikawa, A. Minamino, A. Okada, A. Sarrat, A. Suzuki, A.T. Suzuki, C.K. Jung, C. Mauger, C. McGrew, C. Mitsuda, C. Saji, C.W. Sterner, C.W. Walter, C. Yanagisawa, D. Casper, D. Kielczewska, D. Takemori, D. Turcan, D.W. Liu, E. Blaufuss, E. Kearns, E. Sharkey, G. Guillian, G.W. Sullivan, H.I. Kim, H. Ishino, H.K. Seo, H. Maesaka, H. Okazawa, H. Takeuchi, H.W. Sobel, I. Kato, I.T. Lim, J.A. Goodman, J.G. Learned, J. Hill, J. Kameda, J.L. Stone, J.P. Cravens, J. Shirai, J.Y. Kim, J. Zalipska, K. Hayashi, K. Inoue, K. Ishihara, K. Kaneyuki, K. Kobayashi, K.K. Shiraishi, K. Miyano, K. Nakamura, K. Nishijima, K. Nishikawa, K. Nitta, K. Scholberg, K.S. Ganezer, K. Washburn, L.R. Sulak, M.B. Smy, M.D. Messier, M. Earl, M. Goldhaber, M. Hasegawa, M. Ishitsuka, M. Koshiba, M. Malek, M. Miura, M. Morii, M. Nakahata, M.R. Vagins, M. Sakuda, M. Shiozawa, M. Takita, M. Yoshida, N. Sakurai, R. Gran, R.J. Wilkes, R. Nambu, R. Nishimura, R. Svoboda, R.W. Ellsworth, S. Dazeley, S. Fukuda, S. Hatakeyama, S. Matsuno, S. Mine, S. Moriyama, S. Nakayama, S. Tasaka, S. Ueda, Super-Kamiokande Collaboration: S. Desai, S. Yamada, S. Yamamoto, T. Barszczak, T. Harada, T. Hasegawa, T. Hashimoto, T. Inagaki, T. Ishida, T. Ishii, T. Ishizuka, T. Iwashita, T.J. Haines, T. Kajita, T. Kato, T. Kobayashi, T. Maruyama, T. Morita, T. Nakaya, T. Namba, T. Ooyabu, T. Sasaki, T. Shibata, T. Toshito, W.E. Keig, W. Gajewski, W.R. Kropp, W. Wang, Y. Ashie, Y. Choi, Y. Fukuda, Y. Gando, Y. Hayato, Y. Itow, Y. Kajiyama, Y. Koshio, Y. Nagashima, Y. Nakajima, Y. Obayashi, Y. Oyama, Y. Suzuki, Y. Takeuchi, Y. Totsuka, Y. Watanabe. "Search for Dark Matter WIMPs using Upward Through-going Muons in Super-Kamiokande." arXiv:hep-ex/0404025 (2004). https://pith.science/paper/LQ6YSIO4
Cite this reviewBibTeX for Pith's review of this paper
Claim paper

Why Pith says this

Highlight any text to comment on it.

Referee report

How Pith checks papers → · Full audit of this paper →

The paper

The paper claims

Super-Kamiokande finds no high-energy neutrino excess from WIMP annihilation in the Sun, the Earth's core, or the Galactic Center, and turns that null result into upper limits on how strongly dark matter can scatter off nuclei.

The reading

The paper asks a simple question with a hard measurement behind it: if Weakly Interacting Massive Particles are the dark matter, they should pile up in the Sun and the Earth, annihilate in pairs, and send a faint beam of high-energy muon neutrinos toward us from those directions. Using 1679.6 live days of Super-Kamiokande data and 1892 neutrino-induced upward through-going muons, the collaboration counts events inside cones of half-angle 5 to 30 degrees around the Sun, the Earth's center, and the Galactic Center, and compares each count with the atmospheric-neutrino background expected after neutrino oscillations. No cone shows a statistically significant excess, so the result is a set of 90% confidence flux limits rather than a detection. Those limits matter because they can be converted, under a stated and deliberately generous assumption, into upper bounds on the WIMP-nucleon cross-section, which puts an indirect neutrino search on the same axis as the direct-detection experiments that hunt for nuclear recoils in underground detectors.

What carries the argument

The load-bearing device is the mass-dependent angular cone. A WIMP of mass $m_chi$ produces muons whose angular spread about the source is set mainly by the neutrino-muon scattering angle, so light WIMPs give a wide signal and heavy WIMPs a narrow one; the authors use existing simulations to pick, for each mass, the half-angle containing 90% of the signal (about $2^circ$ at 10 TeV and $22^circ$ at 18 GeV for the Earth, $1.5^circ$ and $19^circ$ for the Sun), and correct for the fraction of signal the cone collects. The second device is the maximum direct-to-indirect rate ratio, a quantity built from the second moment of the neutrino energy spectrum summed over annihilation channels, which lets a measured muon flux limit be traded against a nuclear recoil rate without committing to a particular supersymmetric spectrum. Together these convert a counting experiment in a water tank into a statement about dark matter scattering in germanium and sodium iodide detectors.

Extended reading notes

Core claim

The central claim is a null result with teeth: over 1679.6 live days, the observed angular distributions of upward through-going muons about the Sun, the Earth's center, and the Galactic Center show no statistically significant excess over the atmospheric neutrino background in any half-angle cone from 5 to 30 degrees. From each cone the authors extract a 90% confidence upper limit on the excess neutrino-induced muon flux, using $N_{90}$ from the observed and expected counts divided by an exposure $E = A T$. Because the angular size of the expected signal shrinks with WIMP mass, they then choose, for each mass, the cone that would contain 90% of the signal, and plot flux limits from 18 GeV to 10 TeV for all three targets, comparing them with MACRO, Baksan, Kamiokande, IMB, and AMANDA. Finally, using the maximum ratio of direct-detection to indirect-detection rates computed by Kamionkowski and collaborators, they convert the combined Sun-plus-Earth flux limit into a 90% confidence upper limit on the spin-independent WIMP-nucleon cross-section, and the Sun-only limit into a bound on the spin-dependent WIMP-proton cross-section. The scalar limit excludes a significant portion of the region favored by the DAMA annual-modulation claim, and the spin-dependent limit is roughly two orders of magnitude more sensitive than the corresponding direct-detection bounds.

Load-bearing premise

The step from a measured muon flux limit to a WIMP-nucleon cross-section limit rests on the claim that the maximum ratio of direct to indirect detection rates computed elsewhere is a true upper bound for any neutralino, and the authors themselves note it can fail for WIMPs that annihilate mainly to Higgs bosons or gluons.

Editorial extensions

If this is right

  • Any WIMP model whose spin-independent cross-section and mass place it inside the region excluded in the paper's scalar-coupling figure is inconsistent with the Super-K upward muon data, given the stated conversion assumptions.
  • The spin-dependent WIMP-proton limits derived from the Sun-only flux limit reach roughly $10^{-36}$ to $10^{-34}$ cm$^2$ over the 18 GeV to 10 TeV range, about 100 times below the direct-detection bounds shown, so upward muon detectors are the more sensitive probe of axial-vector coupling to protons.
  • The annual modulation reported by DAMA cannot be ascribed to a WIMP with axial-vector coupling to protons, since that parameter space is closed by null solar WIMP searches.
  • Larger exposures and lower muon energy thresholds would tighten the flux limits proportionally, since the limits scale as $N_{90}/E$ with the effective area and livetime.
  • The three targets probe different physics: the Earth is sensitive to spin-independent coupling with a resonance near the iron mass, the Sun to both scalar and axial-vector coupling through hydrogen, and the Galactic Center to the inner halo density profile.

Reading between the lines

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

  • The dip near 56 GeV in the scalar cross-section limit is a capture resonance where the WIMP mass matches an abundant nucleus in the Earth, so the shape of the exclusion curve encodes the composition of the Earth as much as it encodes dark matter; a different assumed elemental abundance profile would move that feature.
  • The discontinuities at roughly 80 GeV and 174 GeV are artifacts of switching which annihilation channel supplies the lower bound on the spectral second moment, which means a reader comparing this curve to a direct-detection curve should compare within a mass band, not across the jumps.
  • The same cone-optimization logic applies directly to future large water Cherenkov and ice detectors: a modest gain in effective area at high energy buys a proportional gain in cross-section reach, so the natural next step is a joint cone-based stacking of Sun, Earth, and Galactic Center rather than separate limits.
  • Because the conversion assumes the maximum rate ratio is an upper bound, any WIMP whose annihilation runs predominantly to Higgs bosons or gluons could sit outside the quoted exclusion without contradiction, which is a testable loophole for model builders rather than a defect of the data.
Original abstract

We present the results of indirect searches for Weakly Interacting Massive Particles (WIMPs) with 1679.6 live days of data from the Super-Kamiokande detector using neutrino-induced upward through-going muons. The search is performed by looking for an excess of high energy muon neutrinos from WIMP annihilations in the Sun, the core of the Earth, and the Galactic Center, as compared to the number expected from the atmospheric neutrino background. No statistically significant excess was seen. We calculate flux limits in various angular cones around each of the above celestial objects. We obtain conservative model-independent upper limits on WIMP-nucleon cross-section as a function of WIMP mass and compare these results with the corresponding results from direct dark matter detection experiments.

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.

Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 4,313 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.02 · states limitation 0.51 · human participants 0.02 · controlled comparison 0.74 · randomized assignment 0.01 · states quantitative result 0.60 · compares with prior results 0.95 · mentions code or data availability 0.02.

The abstract, sentence by sentence

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

We present the results of indirect searches for Weakly Interacting Massive Particles (WIMPs) with 1679.6 live days of data from the Super-Kamiokande detector using neutrino-induced upward through-going muons. The search is performed by looking for an excess of high energy muon neutrinos from WIMP annihilations in the Sun, the core of the Earth, and the Galactic Center, as compared to the number expected from the atmospheric neutrino background. No statistically significant excess was seen. We calculate flux limits in various angular cones around each of the above celestial objects. We obtain conservative model-independent upper limits on WIMP-nucleon cross-section as a function of WIMP mass and compare these results with the corresponding results from direct dark matter detection experiments.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 We present the results of indirect searches for Weakly Interacting Massive Particles (WIMPs) with 1679.6 live days of data from the Super-Kamiokande detector using neutrino-induced upward through-going muons. contribution 0.87 0.97 0.05 asserted 0.99
s1 The search is performed by looking for an excess of high energy muon neutrinos from WIMP annihilations in the Sun, the core of the Earth, and the Galactic Center, as compared to the number expected from the atmospheric neutrino background. method 0.99 0.90 0.04 asserted 0.98
s2 No statistically significant excess was seen. result 1.00 0.96 0.87 asserted 1.00
s3 We calculate flux limits in various angular cones around each of the above celestial objects. method 0.74 0.96 0.02 asserted 0.99
s4 We obtain conservative model-independent upper limits on WIMP-nucleon cross-section as a function of WIMP mass and compare these results with the corresponding results from direct dark matter detection experiments. result 0.92 0.96 0.16 asserted 1.00

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.51.

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

Figures
Figure 2. FIG. 2: Angular distribution of upward through-going muons
Figure 3. FIG. 3: Angular distribution of upward through-going muons
Figure 4. FIG. 4: The expanded view of the zenith angle distribution
Figure 7. FIG. 7: Comparison of Super-K 90 % CL excess neutrino
Figure 8. FIG. 8: Comparison of Super-K 90 % CL excess neutrino
Figure 9. FIG. 9: Comparison of Super-K 90 % CL excess neutrino
Figure 11. FIG. 11: Super-K WIMP-induced upward muon flux limits
Figure 12. FIG. 12: Super-K WIMP-induced upward muon flux limits
Figure 13. FIG. 13: Super-K 90 % CL exclusion region in WIMP pa
Figure 14. FIG. 14: Super-K 90 % CL exclusion region in WIMP param

Showing 10 of the paper's 14 figures. See all figures in the PDF ↗ Figures reproduced from arXiv:hep-ex/0404025 by the authors.

References
How later papers used it

103 later papers cite it

Evidence: substantial. 94 of the citing papers share no author with it, and 30 of those carry a confident label from Pith's citation classifier.

Pith read 32 of the 146 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

Uses its data or values 4 of 22 papers with this label
Compares with it 3 of 11 papers with this label

  • Compared its predicted muon fluxes with the respective upper limit obtained by Super-Kamiokande in this paper, relating to an angle of 10 degrees around the Solar center.

    Muon Flux Limits for Majorana Dark Matter Particles (2008) · 0.88 · paraphrased: the licence does not allow quoting

  • Computed the total muon flux predicted from its model and confronted it with the Super-Kamiokande bounds from this paper.

    Dark Matter Through the Neutrino Portal (2009) · 0.93 · paraphrased: the licence does not allow quoting

  • Found that its best fit model's neutrino flux as a function of opening angle around the GC is consistent with the bounds of this paper.

    Searching for Smoking Gun Signatures of Decaying Dark Matter (2009) · 0.95 · paraphrased: the licence does not allow quoting

How the literature uses it

99 arXiv papers cite this in 142 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 2 papers

Papers citing it · 89 sentences without a confident label

Uses its data or values 22 papers
Compares with it 10 papers
Cites it as background 16 papers
  • Additionally, Super Kamiokande [ref] , AMANDA [ref] and IceCube [ref] have published limits on localized decay for dark matter particle masses around $∼1 - 10^4$ GeV.

    Using Secondary Tau Neutrinos to Probe Heavy Dark Matter Decays in Earth · Introduction · 0.85

  • Searches have also been conducted for neutrinos that could be produced through dark matter annihilation in the core of the Sun [ref] .

    Searching for dark matter annihilation in the Sun with the IceCube Upgrade · Introduction · 0.95

  • While a great deal of the parameter space for neutral LOLIPs is unexplored, some constraints already exists. �Collider constraints from low energy experiments have been covered in many different ways in [ref] . �However, if DM particles can annihilate into LOLIPs there are additional indirect constraints on some part of the parameter space. �These constraints roughly fall into three categories: existing neutrino telescope bounds, photon and electron fluxes from the Sun, and DM direct detection experiments. � If the LOLIPs subsequently decay into muons, then SuperK bounds from up-going muon searches from both the Sun and the Earth are relevant [ref] . �As explained in Section [ref], these searches are just a rough bound on the LOLIP scenario because utilize on neutrino induced muon events in SuperK. �

    Searches for Long Lived Neutral Particles · Existing Constraints · 0.92

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.