Atmospheric Neutrinos

Useful Links

References

Useful Links

Atmospheric Neutrino Experiments.

Review of Particle Physics: Cosmic Rays

The FLUKA 3-D Atmospheric Neutrino Flux, tables of calculated fluxes (see hep-ph/9907408)

Evidence for Neutrino Mass from Observations of Atmospheric Neutrinos with Super-Kamiokande Ph.D. Thesis by Mark D. Messier

Atmospheric neutrino oscillation analysis using FLUKA 3D flux and Super-Kamiokande data, Atsuko Kibayashi, PhD Thesis, University of Hawaii, August 2002

APS Neutrino Study: Solar and Atmospheric Neutrino Experiments Working Group

Nuance Neutrino Generator

L/E analysis of the atmospheric neutrino data from Super-Kamiokande, Masaki Ishitsuka, PhD Thesis, University of Tokyo, Feb. 2004

Atmosphere

Physics of Atmospheres and Oceans

References

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[1-4]

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[2-1]

MINOS neutrino oscillation results, Habig, Alec, Mod. Phys. Lett. A25 (2010) 1219-1231, arXiv:1004.2647.

[2-2]

Discovery of neutrino oscillations, Kajita, T., Rept. Prog. Phys. 69 (2006) 1607-1635.

[2-3]

Atmospheric neutrinos, Kajita, T., New J. Phys. 6 (2004) 194. http://www.iop.org/EJ/abstract/1367-2630/6/1/194.

[2-4]

Astrophysical Neutrino Telescopes, A. B. McDonald et al., Rev. Sci. Instrum. 75 (2004) 293, arXiv:astro-ph/0311343.
Comment: The figure n. 19 shows the 90 % C.L. allowed contours for oscillations obtained by different atmospheric neutrino experiments. [M.L.].

[2-5]

Oscillations of atmospheric neutrinos, Jung, C. K., McGrew, C., Kajita, T., Mann, T., Ann. Rev. Nucl. Part. Sci. 51 (2001) 451-488.
From the article: The observation made by the Super-Kamiokande experiment of muon flavor disappearance in the atmospheric neutrino flux provides compelling evidence for neutrino flavor oscillations and, by implication, for nonzero neutrino rest mass. In the Standard Model neutrinos are assumed to be massless. However, the quantum-mechanical phenomenon of neutrino oscillations requires neutrinos to have a nonzero rest mass. Consequently, the Super-Kamiokande observations alter our view of these fundamental leptons and have profound implications for elementary particle physics, cosmology and astrophysics. Ultimately, the Standard Model must be modified to accomodate this result.

[2-6]

Observation of atmospheric neutrinos, Kajita, T., Totsuka, Y., Rev. Mod. Phys. 73 (2001) 85-118.

[2-7]

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Muon Neutrino Disappearance and Tau Neutrino Appearance, M. C. Sanchez, arXiv:1112.0618, 2011. XXXI Conference on Physics in Collision, Vancouver, Canada, August 28 to September 1, 2011.

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[3-4]

Atmospheric neutrino oscillations, Giacomelli, G., Giorgini, M. (the MACRO), arXiv:hep-ex/0504002, 2005. 7th School on Non-Accelerator Astroparticle Physics, Trieste, Italy, 2004.

[3-5]

Evidence for Neutrino Mass: A Decade of Discovery, K.M. Heeger, arXiv:hep-ex/0412032, 2004. SEESAW25: International Conference on the Seesaw Mechanism and Neutrino Mass, Paris, France, 10-11 June 2004.

[3-6]

Recent Results of non-accelarator-based neutrino experiments, Yifang Wang, Int. J. Mod. Phys. A20 (2005) 5244, arXiv:hep-ex/0411028. "32nd International Conference on High Energy Physics", Aug. 16-22, 2004, Beijing, P.R. China.

[3-7]

Neutrinos underground, Sobel,H., 2004. AAAS meeting 2004, 17-21 Feb. 2004, Washington, DC, US. http://harv11.fnal.gov/~smaria/aaas04/hank_aaas04.pdf.

[3-8]

Neutrino Physics: Experimental Status, Kajita, T., 2003. 19th International Workshop on Weak Interactions and Neutrinos, WIN2003, October 6-11, Lake Geneva, Wisconsin, USA. http://conferences.fnal.gov/win03/Talks/Takaaki%20Kajita.pdf.
Comment: The slide n. 19 shows the C.L. allowed contours for oscillations obtained by different atmospheric neutrino experiments. The figure in slide n.24 shows the C.L. allowed contour for oscillations obtained by Super-Kamiokande. [M.L.].

[3-9]

Results and status of current accelerator neutrino experiments, Nishikawa, K., 2003. XXI International Symposium on Lepton Photon 2003, 11-16 August 2003, Fermi National Accelerator Laboratory, Batavia, Illinois, USA. http://conferences.fnal.gov/lp2003/program/S10/nishikawa_s10.pdf.
Comment: The slide n.40 shows the expected sensitivity on of different projects. [M.L.].

[3-10]

Atmospheric Neutrinos in 2002, Kearns, Edward T., Frascati Phys. Ser. 28 (2002) 413-426, arXiv:hep-ex/0210019. Heavy Quarks and Leptons 2002, Vietri sul Mare, Italy, May 27-June 1, 2002. http://hep.bu.edu/~kearns/pub/kearns-atmnu2002-hql.pdf.
From the article: ... recent developments in neutrino flux calculation is a key input to more detailed understanding of the data.... in neutrino oscillation studies the flux normalization is allowed to float as a free parameter.
Comment: In Ref.[Fukuda and others, Phys. Rev. Lett.81, 1562 (1998)] the overall normalization was estimated to have a 25% uncertainty but was fitted as a free parameter. An interesting question is whether now, after recent Monte Carlo calculations, the error on the total normalization could be reduced of a relevant factor and be used in the fit of neutrino oscillation studies.
Slide n.9 shows results of SK Fit using 3D Flux Calculations.
(M.L.).

[3-11]

Atmospheric and long baseline neutrino, Nakaya, T. (Super-Kamiokande), eConf C020620 (2002) SAAT01, arXiv:hep-ex/0209036. 22nd Physics in Collision Conference (PIC 2002), Stanford, California, 20-22 June 2002.

[3-12]

Atmospheric Neutrinos and K2K, Nishikawa, K., 2002. Topical Seminar on Frontier of Particle Physics 2002: Neutrinos and Cosmology, 20-25 August 2002, Beijing, China. http://bes.ihep.ac.cn/particle/2002/presentation/K.Nishikawa/TALK_2.ZIP.

[3-13]

Status and prospects of neutrino oscillations: Atmospheric, Kajita, T., 2002. Fourth NuFact '02 Workshop on Neutrino Factories based on Muon Storage Rings, Imperial College, London, 1-6 July 2002. http://www.hep.ph.ic.ac.uk/NuFact02/Scientific-programme/files/Monday/plenary/A03_kajita.ppt.

[3-14]

Experimental measurements of atmospheric neutrinos, Kearns, Edward, Nucl. Phys. Proc. Suppl. 70 (1999) 315-323, arXiv:hep-ex/9803007.

[4-1]

Phenomenology with Massive Neutrinos, Gonzalez-Garcia, M. C., Maltoni, Michele, Phys. Rept. 460 (2008) 1-129, arXiv:0704.1800.

[4-2]

Global analysis of three-flavor neutrino masses and mixings, Fogli, G. L., Lisi, E., Marrone, A., Palazzo, A., Prog. Part. Nucl. Phys. 57 (2006) 742-795, arXiv:hep-ph/0506083.

[4-3]

Atmospheric neutrinos and neutrino oscillations, Takaaki Kajita, Paolo Lipari, Comptes Rendus Physique 6 (2005) 739-748.

[4-4]

Report of the Solar and Atmospheric Neutrino Experiments Working Group of the APS Multidivisional Neutrino Study, H. Back et al., arXiv:hep-ex/0412016, 2004.

[4-5]

Neutrino Masses and Oscillations: Triumphs and Challenges, R.D. McKeown, P. Vogel, Phys. Rep. 394 (2004) 315, arXiv:hep-ph/0402025.

[4-6]

Cosmic rays, Gaisser, T. K., Stanev, T., Phys. Lett. B592 (2004) 228-234. The Review of Particle Properties 2004. http://pdg.lbl.gov/2004/reviews/cosmicrayrpp.pdf.

[4-7]

Neutrino Mixing, Carlo Giunti, Marco Laveder, arXiv:hep-ph/0310238, 2003. In "Developments in Quantum Physics - 2004", p. 197-254, edited by F. Columbus and V. Krasnoholovets, Nova Science, Hauppauge, NY. http://novapublishers.com/catalog/product_info.php?products_id=1633.

[4-8]

Flux of Atmospheric Neutrinos, Gaisser, T. K., Honda, M., Ann. Rev. Nucl. Part. Sci. 52 (2002) 153, arXiv:hep-ph/0203272.
From the article: An offset in normalization of the neutrino flux does not affect the conclusions about oscillations, which are robust. Nevertheless, it is interesting and informative to compare the measured neutrino flux as directly as possible in an absolute fashion with the calculations. Fig. 25 at page 58 compares the neutrino fluxes measured at Super-K with the two calculations [,15-42] that have been used extensively as input to the detector simulation. The comparisons are made as a function of visible energy by the Super-K group. The magnitudes are consistent with what is expected for oscillations in this energy range that involve and but not ; namely, there is a deficit of , whereas the measured flux of electron neutrinos is consistent with the calculation.

[4-9]

Neutrino Masses and Mixing: Evidence and Implications, M.C. Gonzalez-Garcia, Y. Nir, Rev. Mod. Phys. 75 (2003) 345-402, arXiv:hep-ph/0202058.

[4-10]

Finally neutrino has mass?, Bilenky, S. M., Giunti, C., Kim, C. W., Int. J. Mod. Phys. A15 (2000) 625-650, arXiv:hep-ph/9902462.

[4-11]

Phenomenology of neutrino oscillations, S. M. Bilenky, C. Giunti, W. Grimus, Prog. Part. Nucl. Phys. 43 (1999) 1, arXiv:hep-ph/9812360.

[4-12]

Cosmic ray showers, Greisen, K., Ann. Rev. Nucl. Part. Sci. 10 (1960) 63-108.

[5-1]

Muons and Neutrinos 2007, Thomas K. Gaisser, arXiv:0801.4542, 2008. 30th International Cosmic Ray Conference, Merida, Yucatan, July, 2007.

[5-2]

Atmospheric Neutrinos, Thomas K. Gaisser, AIP Conf. Proc. 944 (2007) 140-142, arXiv:astro-ph/0612274. Neutrino 2006.

[5-3]

Global fits to neutrino oscillation data, Thomas Schwetz, Phys. Scripta T127 (2006) 1-5, arXiv:hep-ph/0606060. SNOW2006 workshop, Stockholm, 2-6 May 2006.

[5-4]

Neutrino oscillations: Current status and prospects, Thomas Schwetz, Acta Phys. Polon. B36 (2005) 3203, arXiv:hep-ph/0510331. XXIX International Conference of Theoretical Physics, "Matter To The Deepest: Recent Developments In Physics of Fundamental Interactions", 8-14 September 2005, Ustron, Poland.

[5-5]

Neutrino mass and mixing parameters: A short review, G.L. Fogli et al., arXiv:hep-ph/0506307, 2005. 40th Rencontres de Moriond on Electroweak Interactions and Unified Theories, La Thuile, Aosta Valley, Italy, 5-12 Mar 2005.

[5-6]

Atmospheric neutrino challenges, Todor Stanev, Nucl. Phys. Proc. Suppl. 145 (2005) 69, arXiv:astro-ph/0412395. NOW 2004.

[5-7]

Three-flavour effects and CP- and T-violation in neutrino oscillations, Evgeny Akhmedov, Phys. Scripta T121 (2005) 65, arXiv:hep-ph/0412029. Nobel Symposium 129 - Neutrino Physics, Haga Slott, Enkoping, Sweden, August 19-24, 2004.

[5-8]

Physics of Massive Neutrinos, J. W. F. Valle, Nucl. Phys. Proc. Suppl. 149 (2005) 3, arXiv:hep-ph/0410103. Sixth International Conf. on Neutrino Factories and SuperBeams (NuFact04) Osaka, Japan, July 26-August 1, 2004.

[5-9]

Neutrino 2004: Concluding Talk, Guido Altarelli, Nucl. Phys. Proc. Suppl. 143 (2005) 470, arXiv:hep-ph/0410101. Neutrino 2004, Paris, 14-19 June 2004.

[5-10]

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[5-11]

Global analysis of neutrino oscillation, S. Goswami, 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/tuesday/goswami.pdf.

[5-12]

Neutrino physics, recent results, Lisi, E., 2004. IFAE-2004, 14-16 April 2004, Torino, Italy. http://agenda.cern.ch/askArchive.php?base=agenda&categ=a041654&id=a041654s3t6/transparencies, http://www.ph.unito.it/ifae/Proceedings/Sessioni/Neutrinos.pdf.

[5-13]

Neutrino masses twenty-five years later, Valle, J W F, Aip Conf. Proc. 687 (2003) 16, arXiv:hep-ph/0307192. MRST'03 (Joe-Fest), Syracuse, NY, May 2003.

[5-14]

Neutrino oscillations in the framework of the tree-neutrino mixing, Bilenky, S. M., arXiv:hep-ph/0307186, 2003. Ist Yamada Symposium Om neutrinos and Dark Matter in Nuclear Physics, June 9-14, 2003, Nara, Japan.

[5-15]

Neutrino Physics after KamLAND, Smirnov, Alexei Yu., arXiv:hep-ph/0306075, 2003. 4th Workshop on "Neutrino Oscillations and their Origin" (NOON2003), February 10-14, 2003, Ishikawa Kousei Nenkin Kaikan, Kanazawa, Japan. http://www-sk.icrr.u-tokyo.ac.jp/noon2003/transparencies/10/Smirnov.pdf.

[5-16]

Status of Neutrino Fits, C. Giunti, arXiv:hep-ph/0305139, 2003. XXXVIIIth Rencontres de Moriond, ElectroWeak Interactions and Unified Theories, 15-22 March 2003, Les Arcs, France. http://moriond.in2p3.fr/EW/2003/Transparencies/1_Sunday/1_2_afternoon/1_2_6_Giunti/C.Giunti.pdf.

[5-17]

Neutrino Masses and Mixing: Where We Stand and Where We are Going, M. C. Gonzalez-Garcia, arXiv:hep-ph/0211054, 2002. 10th International Conference on Supersymmetry and Unification of Fundamental Interactions, SUSY02 (June 17-23, 2002, DESY, Hamburg).

[5-18]

Theory of Neutrino Masses and Mixing, M.C. Gonzalez-Garcia, Nucl. Phys. Proc. Suppl. 117 (2003) 186, arXiv:hep-ph/0210359. 31st international conference on high energy physics (ICHEP 2002), Amsterdam, 24-31 July 2002.

[5-19]

Current Status of Neutrino Masses and Mixings, Giunti, C., arXiv:hep-ph/0209103, 2002. 31st International Conference on High Energy Physics "ICHEP02", 24-31 July 2002, Amsterdam. http://www.ichep02.nl/Transparencies/NEU/NEU-2/NEU-2-1.giunti.ps.

[6-1]

First Evidence For Atmospheric Neutrino-Induced Cascades with the IceCube Detector, Michelangelo D'Agostino, arXiv:0910.2555, 2009.

[7-1]

Study of Non-Standard Neutrino Interactions with Atmospheric Neutrino Data in Super-Kamiokande I and II, G. Mitsuka et al. (Kamiokande), Phys. Rev. D84 (2011) 113008, arXiv:1109.1889.

[7-2]

Search for Differences in Oscillation Parameters for Atmospheric Neutrinos and Antineutrinos at Super-Kamiokande, K. Abe et al. (Super-Kamiokande), Phys. Rev. Lett. 107 (2011) 241801, arXiv:1109.1621.

[7-3]

First search for atmospheric and extraterrestrial neutrino-induced cascades with the IceCube detector, R. Abbasi et al. (IceCube), Phys. Rev. D84 (2011) 072001, arXiv:1101.1692.

[7-4]

Measurement of the atmospheric neutrino energy spectrum from 100 GeV to 400 TeV with IceCube, R. Abbasi et al. (IceCube), Phys. Rev. D83 (2011) 012001, arXiv:1010.3980.

[7-5]

The first search for extremely-high energy cosmogenic neutrinos with the IceCube Neutrino Observatory, R. Abbasi et al. (IceCube), Phys. Rev. D82 (2010) 072003, arXiv:1009.1442.

[7-6]

The Energy Spectrum of Atmospheric Neutrinos between 2 and 200 TeV with the AMANDA-II Detector, R. Abbasi et al. (IceCube), Astropart. Phys. 34 (2010) 48-58, arXiv:1004.2357.

[7-7]

Atmospheric neutrino oscillation analysis with sub-leading effects in Super-Kamiokande I, II, and III, R. Wendell et al. (Super-Kamiokande), Phys. Rev. D81 (2010) 092004, arXiv:1002.3471.

[7-8]

Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory, Collaboration, SNO (SNO), Phys. Rev. D80 (2009) 012001, arXiv:0902.2776.

[7-9]

Determination of the Atmospheric Neutrino Flux and Searches for New Physics with AMANDA-II, Collaboration, The IceCube (IceCube), Phys. Rev. D79 (2009) 102005, arXiv:0902.0675.

[7-10]

Kinematic reconstruction of atmospheric neutrino events in a large water Cherenkov detector with proton identification, M. Fechner et al. (Super-Kamiokande), Phys. Rev. D79 (2009) 112010, arXiv:0901.1645.

[7-11]

Search for Matter-Dependent Atmospheric Neutrino Oscillations in Super-Kamiokande, K. Abe et al. (Super-Kamiokande), Phys. Rev. D77 (2008) 052001, arXiv:0801.0776.

[7-12]

Experimental study of the atmospheric neutrino backgrounds for proton decay to positron and neutral pion searches in water Cherenkov detectors, S. Mine et al. (K2K), Phys. Rev. D77 (2008) 032003, arXiv:0801.0182.

[7-13]

Detection of Atmospheric Muon Neutrinos with the IceCube 9-String Detector, A. Achterberg et al. (IceCube), Phys. Rev. D76 (2007) 027101, arXiv:0705.1781.

[7-14]

Charge-Separated Atmospheric Neutrino-Induced Muons in the MINOS Far Detector, P. Adamson et al. (MINOS), Phys. Rev. D75 (2007) 092003, arXiv:hep-ex/0701045.

[7-15]

A Measurement of Atmospheric Neutrino Flux Consistent with Tau Neutrino Appearance, K. Abe et al. (Super-Kamiokande), Phys. Rev. Lett. 97 (2006) 171801, arXiv:hep-ex/0607059.
From the abstract: The Super-Kamiokande-I atmospheric neutrino data for 1489.2 days, which find a best fit tau neutrino appearance signal of , disfavor the hypothesis of no tau neutrino appearance by 2.4 sigma.

[7-16]

Three flavor neutrino oscillation analysis of atmospheric neutrinos in Super-Kamiokande, J. Hosaka et al. (Super-Kamiokande), Phys. Rev. D74 (2006) 032002, arXiv:hep-ex/0604011.

[7-17]

First Observations of Separated Atmospheric Muon Neutrino and Muon Anti-Neutrino Events in the MINOS Detector, P. Adamson et al. (MINOS), Phys. Rev. D73 (2006) 072002, arXiv:hep-ex/0512036.
From the abstract: The ratio of upward to downward-going events in the data is compared to the Monte Carlo expectation in the absence of neutrino oscillations giving: ... The ratio of to events in the data is compared to the Monte Carlo expectation assuming neutrinos and anti-neutrinos oscillate in same manner giving: ... Although the statistics are limited, this is the first direct observation of atmospheric neutrino interactions separately for and .

[7-18]

Neutrino Oscillation Effects in Soudan-2 Upward-stopping muons, Allison, W. W. M. et al. (Soudan-2), Phys. Rev. D72 (2005) 052005, arXiv:hep-ex/0507068.

[7-19]

A Measurement of Atmospheric Neutrino Oscillation Parameters by Super-Kamiokande I, Y. Ashie et al. (Super-Kamiokande), Phys. Rev. D71 (2005) 112005, arXiv:hep-ex/0501064.

[7-20]

Evidence for an oscillatory signature in atmospheric neutrino oscillation, Y. Ashie et al. (Super-Kamiokande), Phys. Rev. Lett. 93 (2004) 101801, arXiv:hep-ex/0404034.
From the abstract: Muon neutrino disappearance probability as a function of neutrino flight length over neutrino energy was studied.
A dip in the distribution was observed in the data, as predicted from the sinusoidal flavor transition probability of neutrino oscillation.
The observed distribution constrained neutrino oscillation parameters; and at 90% confidence level.

[7-21]

Observation of Atmospheric Neutrino Oscillations in Soudan 2, M. Sanchez et al. (Soudan 2), Phys. Rev. D68 (2003) 113004, arXiv:hep-ex/0307069.

[7-22]

Atmospheric neutrino oscillations from upward throughgoing muon multiple scattering in MACRO, M. Ambrosio et al. (MACRO), Phys. Lett. B566 (2003) 35, arXiv:hep-ex/0304037.

[7-23]

Matter effects in upward-going muons and sterile neutrino oscillations, Ambrosio, M. et al. (MACRO), Phys. Lett. B517 (2001) 59-66, arXiv:hep-ex/0106049.

[7-24]

Tau neutrinos favored over sterile neutrinos in atmospheric muon neutrino oscillations, Fukuda, S. et al. (Super-Kamiokande), Phys. Rev. Lett. 85 (2000) 3999-4003, arXiv:hep-ex/0009001.

[7-25]

Low energy atmospheric muon neutrinos in MACRO, Ambrosio, M. et al. (MACRO), Phys. Lett. B478 (2000) 5-13.

[7-26]

The atmospheric neutrino flavor ratio from a 3.9 fiducial kiloton-year exposure of Soudan 2, Allison, W. W. M. et al. (Soudan-2), Phys. Lett. B449 (1999) 137-144, arXiv:hep-ex/9901024.

[7-27]

Measurement of the flux and zenith-angle distribution of upward through-going muons by Super-Kamiokande, Fukuda, Y. et al. (Super-Kamiokande), Phys. Rev. Lett. 82 (1999) 2644-2648, arXiv:hep-ex/9812014.

[7-28]

Measurement of the atmospheric neutrino-induced upgoing muon flux using MACRO, Ambrosio, M. et al. (MACRO), Phys. Lett. B434 (1998) 451-457, arXiv:hep-ex/9807005.

[7-29]

Evidence for oscillation of atmospheric neutrinos, Fukuda, Y. et al. (Super-Kamiokande), Phys. Rev. Lett. 81 (1998) 1562-1567, arXiv:hep-ex/9807003.

[7-30]

Measurement of the flux and zenith angle distribution of upward through-going muons in Kamiokande II + III, Hatakeyama, S. et al. (Kamiokande), Phys. Rev. Lett. 81 (1998) 2016-2019, arXiv:hep-ex/9806038.

[7-31]

Study of the atmospheric neutrino flux in the multi-GeV energy range, Fukuda, Y. et al. (Super-Kamiokande), Phys. Lett. B436 (1998) 33-41, arXiv:hep-ex/9805006.

[7-32]

Measurement of a small atmospheric nu/mu / nu/e ratio, Fukuda, Y. et al. (Super-Kamiokande), Phys. Lett. B433 (1998) 9-18, arXiv:hep-ex/9803006.

[7-33]

The Baksan underground scintillation telescope, Alekseev, E. N. et al., Phys. Part. Nucl. 29 (1998) 254-256.

[7-34]

Atmospheric muon-neutrino fraction above 1-GeV, Clark, R. et al. (IMB), Phys. Rev. Lett. 79 (1997) 345-348.

[7-35]

Study of neutron background in the atmospheric neutrino sample in Kamiokande, Fukuda, Y. et al. (Kamiokande), Phys. Lett. B388 (1996) 397-401.

[7-36]

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[7-37]

Atmospheric muon-neutrino / electron-neutrino ratio in the multiGeV energy range, Fukuda, Y. et al. (Kamiokande), Phys. Lett. B335 (1994) 237-245.

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IMB-3: A Large water Cerenkov detector for nucleon decay and neutrino interactions, Becker-Szendy, R. et al. (IMB), Nucl. Instrum. Meth. A324 (1993) 363-382.

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Survey of atmospheric neutrino data and implications for neutrino mass and mixing, Beier, E. W. et al., Phys. Lett. B283 (1992) 446-453.

[7-40]

Observation of a small atmospheric ratio in Kamiokande, Hirata, K. S. et al. (Kamiokande), Phys. Lett. B280 (1992) 146-152.

[7-41]

A Search for muon-neutrino oscillations with the IMB detector, Becker-Szendy, R. et al. (IMB), Phys. Rev. Lett. 69 (1992) 1010-1013.

[7-42]

The electron-neutrino and muon-neutrino content of the atmospheric flux, Becker-Szendy, R. et al. (IMB), Phys. Rev. D46 (1992) 3720-3724.

[7-43]

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[7-44]

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[7-45]

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Neutrino backgrounds in the Kolar Gold Field nucleon decay experiment, Krishnaswamy, M. r. et al., Pramana 19 (1982) 525-554.

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Limitations on parameters of neutrino oscillations according to data of the baksan underground telescope, Boliev, M. M. et al., Yad. Fiz. 34 (1981) 1418-1421. In Russian.

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Krishnaswamy, M. R. et al., Proc. R. Soc. London A323 (1971) 489.

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Muons produced by atmospheric neutrinos: Analysis, Chen, H. H., Kropp, W. R., Sobel, H. W., Reines, F., Phys. Rev. D4 (1971) 99-121.

[7-65]

Muons produced by atmospheric neutrinos: Experiment, Reines, F. et al., Phys. Rev. D4 (1971) 80-98.

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[8-1]

The First Year IceCube-DeepCore Results, Chang Hyon Ha (IceCube), arXiv:1201.0801, 2012. TAUP 2011.

[8-2]

Results from Super-Kamiokande, Yasuo Takeuchi (Super-Kamiokande), arXiv:1112.3425, 2011. XXIV International Conference on Neutrino Physics and Astrophysics (Neutrino 2010).

[8-3]

The IceCube Neutrino Observatory VI: Neutrino Oscillations, Supernova Searches, Ice Properties, R. Abbasi et al. (IceCube), arXiv:1111.2731, 2011. 32nd International Cosmic Ray Conference, Beijing 2011.

[8-4]

IceCube3-a new window on the Universe, Thomas K. Gaisser, Denis Robertson (IceCube), AIP Conf. Proc. 1123 (2009) 177-189, arXiv:0901.4294. 3rd Latin American School on Cosmic Rays, Arequipa, Peru, September, 2008.

[8-5]

Neutrino Oscillation Measurements with IceCube, Carsten Rott (IceCube), arXiv:0810.3698, 2008. ICHEP08.

[8-6]

Recent Results from Super-Kamiokande, Sekiya, H. et al. (Super-Kamiokande), arXiv:0810.0595, 2008. ICHEP08, Philadelphia, USA, July 2008.

[8-7]

The Super-Kamiokande Experiment, C.W. Walter, arXiv:0802.1041, 2008. Neutrino Oscillations: Present Status and Future Plans.

[8-8]

The MACRO Experiment at Gran Sasso, G. Giacomelli, A. Margiotta, arXiv:0707.1691, 2007. Charles Peck - Fest, Caltech, 2005.

[8-9]

First Results from AMANDA using the TWR System, Andrea Silvestri et al. (IceCube), arXiv:astro-ph/0701319, 2007. International School of Cosmic Ray Astrophysics, 15th Course: 'Astrophysics at Ultra-high Energies', Erice, Italy, 20-27 June 2006.

[8-10]

Neutrino-induced muons observed with MINOS, Habig, Alec T. (MINOS), arXiv:hep-ex/0507010, 2005. 29th International Cosmic Ray Conference (ICRC 2005), Pune, India, 3-11 Aug 2005.

[8-11]

MACRO results on atmospheric neutrinos, G. Giacomelli, A. Margiotta (MACRO), Nucl. Phys. Proc. Suppl. 145 (2005) 116, arXiv:hep-ex/0504029. NOW 2004 Workshop, Conca Specchiulla, Otranto, Italy, September 2004.

[8-12]

Upward Showering Muons in Super-Kamiokande, S. Desai, A. Habig (Super-Kamiokande), 2005. 29th International Cosmic Ray Conference (ICRC 2005), Pune, India, 3-11 Aug 2005. http://budoe.bu.edu/~shantanu/icrc05showering.sxi.pdf.

[8-13]

SuperK recent results, Scholberg, K. (Super-Kamiokande), 2005. 20th International Workshop on Weak Interactions and Neutrinos (WIN'05), June 6-11, 2005, Delphi, Greece. http://conferences.phys.uoa.gr/win05/WIN05_WG3/scholberg.ppt.
Comment: Atmospheric neutrino results from a new (320 bins) analysis are presented. [M.L.].

[8-14]

New MACRO results on atmospheric neutrino oscillations, G. Giacomelli, A. Margiotta (MACRO), Phys. Atom. Nucl. 67 (2004) 1139, arXiv:hep-ex/0407023. NANP03 Int. Conf., Dubna, 2003.

[8-16]

Super Kamiokande results: atmospheric and solar neutrinos, M.Ishitsuka, Super-Kamiokande Collaboration (Super-Kamiokande), arXiv:hep-ex/0406076, 2004. XXXIXth Rencontres de Moriond on Electroweak Interactions (2004).

[8-16]

Super Kamiokande results: atmospheric and solar neutrinos, M.Ishitsuka (Super-Kamiokande), arXiv:hep-ex/0406076, 2004. XXXIX Rencontres de Moriond, Electroweak Interactions and Unified Theories, La Thuile, March 21-28-2004. http://moriond.in2p3.fr/EW/2004/transparencies/3_Wednesday/3_2_afternoon/3_2_3_Ishitsuka/Ishitsuka.pdf.

[8-17]

MACRO results on atmospheric neutrino oscillations, G. Giacomelli, A. Margiotta (MACRO), Eur. Phys. J. C33 (2004) S826, arXiv:hep-ex/0406037. HEP EPS Conf., Aachen, Germany, July 2003.

[8-18]

Other (past, present and future) atmospheric neutrino experiments, H. Gallagher, 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/tuesday/gallagher.ppt.

[8-19]

Atmospheric neutrino results from SuperKamiokande, E. Kearns (Super-Kamiokande), 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/tuesday/kearns.pdf.

[8-20]

Searching for atmospheric neutrino oscillations at MINOS, Blake, A. (MINOS), 2004. UK Institute of Physics: Particle Physics 2004, 5-7 April 2004, Birmingham, UK. http://agenda.cern.ch/askArchive.php?base=agenda&categ=a04837&id=a04837s9t2%2Ftransparencies%2Fblake.pdf.

[8-21]

Direct oscillatory evidence from the L/E analysis in Super-Kamiokande, M. Ishitsuka (Super-Kamiokande), 2004. NOON2004, The 5th Workshop on "Neutrino Oscillations and their Origin", 11-15 February 2004, Tokyo, Japan. http://www-sk.icrr.u-tokyo.ac.jp/noon2004/trape/10-ishitsuka.pdf.
Comment: First oscillation dip is observed in L/E data sample (see this figure).

[8-22]

SK atmospheric neutrino, C. Saji (Super-Kamiokande), 2004. NOON2004, The 5th Workshop on "Neutrino Oscillations and their Origin", 11-15 February 2004, Tokyo, Japan. http://www-sk.icrr.u-tokyo.ac.jp/noon2004/trape/09-Saji.pdf.

[8-23]

Results from the BAIKAL neutrino telescope, R. Wischnewski (The BAIKAL), arXiv:astro-ph/0305302, 2003. 28th International Cosmic Ray Conference, Tsukuda, Japan, July 31 - August 7, 2003.

[8-24]

Atmospheric Neutrino Oscillations in Super-Kamiokande I, Ahabig, A. (Super-Kamiokande), 2003. Talk given at the 28th International Cosmic Ray Conferences (ICRC 2003) 31 Jul - 7 Aug 2003, Tsukuba, Japan. http://neutrino.d.umn.edu/~habig/atmpd.pdf.

[8-25]

Recent results from atmospheric and K2K, Itow, Y., 2003. 2nd International conference on Flavor Physics, ICFP 2003, 6-11 October 2003, Korea Institute for Advanced Study (KIAS). http://newton.kias.re.kr/~hepph/public_html/03icfp/talk/itow1.pdf.
Comment: The figure in slide n.34 shows the K2K excluded region for oscillations of accelerator neutrinos in the channel as compared with the CHOOZ limit and the Super-Kamiokande allowed region. [M.L.].

[10-48]

Status of the Super-Kamiokande, the K2K-2 experiment and JHF nu project, Y. Hayato, 2003. EPS2003. http://eps2003.physik.rwth-aachen.de/data/talks/parallel/07Neutrino/07Hayato.ppt.

[10-50]

New Results from Super-K and K2K, R. Jeffrey Wilkes (K2K), eConf C020805 (2002) TTH02, arXiv:hep-ex/0212035. Secrets of the B-Meson, Topical Conference, XXX SLAC Summer Institute, SLAC, August, 2002.

[8-28]

Other Atmospheric Neutrino Experiments, Goodman, Maury, Nucl. Phys. Proc. Suppl. 118 (2003) 99, arXiv:hep-ex/0210055. XXth International Conference on Neutrino Physics and Astrophysics May 25 - 30, 2002, Munich, Germany. http://neutrino2002.ph.tum.de/pages/transparencies/goodman.

[8-29]

Atmospheric neutrino oscillations with the MACRO detector, M. Giorgini (MACRO), arXiv:hep-ex/0210008, 2002. Beyond the Desert 02, Conference on Physics beyond the Standard Model, Oulu, Finland, 2-7 June 2002.

[8-30]

Neutrino Physics and Astrophysics with the MACRO Experiment at the Gran Sasso Lab, G. Giacomelli (MACRO), Braz. J. Phys. 33 (2003) 211, arXiv:hep-ex/0210006. 25th Meeting of the Nuclear Division of the Brasilian Physical Society, S. Pedro, Brasil, 1-4 September 2002.

[8-31]

Five Years of Neutrino Physics with Super-Kamiokande, M. B. Smy (Super-Kamiokande), arXiv:hep-ex/0206016, 2002. XXXVII Rencontres de Moriond: Electroweak Interactions and Unified Theories.

[8-32]

Atmospheric neutrino oscillations, G. Giacomelli, M. Giorgini, M. Spurio, arXiv:hep-ex/0201032, 2002.

[8-33]

Results from Soudan-2 on Atmospheric Neutrinos and Limits on Matter Instability, Mann, T. (Soudan-2), 2002. Conference on Neutrinos and Implications for Physics Beyond the Standard Model, Stony Brook, Oct. 11-13, 2002. http://insti.physics.sunysb.edu/itp/conf/neutrino/talks/mann.pdf.

[8-34]

Atmospheric Neutrinos at Super-Kamiokande, Mauger, C. (Super-Kamiokande), 2002. 31st International Conference on High Energy Physics - ICHEP 02 - Amsterdam, Holland, 24-31 July 2002. http://www.ichep02.nl/Transparencies/NEU/NEU-1/NEU-1-4.Mauger.pdf.

[8-35]

Experimental results on atmospheric neutrinos in Super-Kamiokande-I, Shiozawa, M. (Super-Kamiokande), 2002. XX^th International Conference on Neutrino Physics and Astrophysics May 25 - 30, 2002, Munich, Germany. http://neutrino2002.ph.tum.de/pages/transparencies/shiozawa.

[8-36]

Atmospheric Neutrinos: Status and Prospects with approved Experiments, Shiozawa, M. (Super-Kamiokande), 2002. Workshop on Large Detectors for proton decay, supernovae, and atmospheric neutrinos, and low energy neutrinos from high intensity beams, NNN02, CERN, 16-18 January 2002. http://muonstoragerings.cern.ch/NuWorkshop02/presentations/shiozawa1.ppt.

[8-37]

Atmospheric Neutrinos, Totsuka, Y., 2001. TAUP2001 - Topics in Astroparticle and Underground Physics, LNGS, Italy (September 8-12, 2001). http://taup2001.lngs.infn.it/f1/f1.pdf.
From the article: Is there a problem in the atmospheric neutrino data of Super-Kamiokande-I when compared with the 3D calculations of G.Battistoni and others [15-30]?.

[8-38]

Experiments with Solar and Atmospheric Neutrinos: Evidence for Neutrino Masses and Lepton Mixing. Experimental status and Future Projects, Schoenert, S., 2001. Astroparticle Physics Workshop, DESY - Zeuten, 19-21 June 2001. http://www.desy.de/desy-hs/zeuthen2001/presentations/main/schoenert.pdf.

[8-39]

Atmospheric neutrino results from Super-Kamiokande, Messier, M. D., Int. J. Mod. Phys. A16S1B (2001) 733-735.

[8-40]

Atmospheric neutrinos at Super-Kamiokande, Scholberg, Kate (Super-Kamiokande), arXiv:hep-ex/9905016, 1999.

[9-1]

Search for Lorentz invariance and CPT violation with muon antineutrinos in the MINOS Near Detector, P. Adamson et al. (The MINOS), arXiv:1201.2631, 2012.

[9-2]

First Muon-Neutrino Disappearance Study with an Off-Axis Beam, K. Abe et al. (T2K), arXiv:1201.1386, 2012.

[9-3]

Indication for the disappearance of reactor electron antineutrinos in the Double Chooz experiment, Y. Abe et al. (DOUBLE-CHOOZ), arXiv:1112.6353, 2011.

[9-4]

Search for the disappearance of muon antineutrinos in the NuMI neutrino beam, P. Adamson et al. (MINOS), Phys. Rev. D84 (2011) 071103, arXiv:1108.1509.

[9-5]

Improved search for muon-neutrino to electron-neutrino oscillations in MINOS, P. Adamson et al. (MINOS), Phys. Rev. Lett. 107 (2011) 181802, arXiv:1108.0015.

[9-6]

Search for oscillation with the OPERA experiment in the CNGS beam, N. Agafonova et al. (OPERA), arXiv:1107.2594, 2011.

[9-7]

Indication of Electron Neutrino Appearance from an Accelerator-produced Off-axis Muon Neutrino Beam, K.Abe et al. (T2K), Phys. Rev. Lett. 107 (2011) 041801, arXiv:1106.2822.

[9-8]

Active to sterile neutrino mixing limits from neutral-current interactions in MINOS, P. Adamson et al. (MINOS), Phys. Rev. Lett. 107 (2011) 011802, arXiv:1104.3922.

[9-9]

First direct observation of muon antineutrino disappearance, Adamson, P. et al. (MINOS), Phys. Rev. Lett. 107 (2011) 021801, arXiv:1104.0344.

[9-10]

Measurement of the neutrino mass splitting and flavor mixing by MINOS, Adamson, P. et al. (MINOS), Phys. Rev. Lett. 106 (2011) 181801, arXiv:1103.0340.

[9-11]

A Search for Lorentz Invariance and CPT Violation with the MINOS Far Detector, Adamson, P. et al. (MINOS), Phys. Rev. Lett. 105 (2010) 151601, arXiv:1007.2791.

[9-12]

Observation of a first candidate in the OPERA experiment in the CNGS beam, N. Agafonova et al. (OPERA), Phys. Lett. B691 (2010) 138-145, arXiv:1006.1623.

[9-13]

New constraints on muon-neutrino to electron-neutrino transitions in MINOS, P. Adamson et al. (MINOS), Phys. Rev. D82 (2010) 051102, arXiv:1006.0996.

[9-14]

Search for sterile neutrino mixing in the MINOS long- baseline experiment, Adamson, P. et al. (The MINOS), Phys. Rev. D81 (2010) 052004, arXiv:1001.0336.

[9-15]

Search for active neutrino disappearance using neutral-current interactions in the MINOS long-baseline experiment, P. Adamson et al. (MINOS), Phys. Rev. Lett. 101 (2008) 221804, arXiv:0807.2424.

[9-16]

Measurement of Neutrino Oscillations with the MINOS Detectors in the NuMI Beam, P. Adamson et al. (MINOS), Phys. Rev. Lett. 101 (2008) 131802, arXiv:0806.2237.

[9-17]

A Study of Muon Neutrino Disappearance Using the Fermilab Main Injector Neutrino Beam, Adamson, P. et al. (MINOS), Phys. Rev. D77 (2008) 072002, arXiv:0711.0769.
From the abstract: We report the results of a search for disappearance by the Main Injector Neutrino Oscillation Search []. The experiment uses two detectors separated by 734 km to observe a beam of neutrinos created by the Neutrinos at the Main Injector facility at Fermi National Accelerator Laboratory.... Based on measurements in the Near Detector, in the absence of neutrino oscillations we expected charged-current interactions at the Far Detector but observed 215. This deficit of events corresponds to a significanc e of 5.2 standard deviations. The deficit is energy dependent and is consistent with two-flavor neutrino oscillations according to and at 68% confidence level.

[9-18]

First CNGS events detected by LVD, N. Yu. Agafonova et al., Eur. Phys. J. C52 (2007) 849-855, arXiv:0710.1536.

[9-19]

First events from the CNGS neutrino beam detected in the OPERA experiment, R. Acquafredda et al. (OPERA), New J. Phys. 8 (2006) 303, arXiv:hep-ex/0611023.

[9-20]

Observation of muon neutrino disappearance with the MINOS detectors and the NuMI neutrino beam, D.G. Michael et al. (MINOS), Phys. Rev. Lett. 97 (2006) 191801, arXiv:hep-ex/0607088.
From the abstract: The data are consistent with muon neutrino disappearance via oscillation with and (68% C.L.).

[9-21]

Measurement of neutrino oscillation by the K2K experiment, Ahn, M. H. et al. (K2K), Phys. Rev. D74 (2006) 072003, arXiv:hep-ex/0606032.

[9-22]

An improved search for oscillation in a long-baseline accelerator experiment, S. Yamamoto et al. (K2K), Phys. Rev. Lett. 96 (2006) 181801, arXiv:hep-ex/0603004.
From the abstract: At , the best fit value of the K2K disappearance analysis, we set an upper limit of at 90% confidence level.

[9-23]

Evidence for muon neutrino oscillation in an accelerator-based experiment, E. Aliu et al. (K2K), Phys. Rev. Lett. 94 (2005) 081802, arXiv:hep-ex/0411038.

[9-24]

Measurement of Neutrino Oscillation with KamLAND: Evidence of Spectral Distortion, T. Araki et al. (KamLAND), Phys. Rev. Lett. 94 (2005) 081801, arXiv:hep-ex/0406035.
From the article: See this summary.

[9-25]

Search for electron neutrino appearance in a 250-km long- baseline experiment, Ahn, M. H. et al. (K2K), Phys. Rev. Lett. 93 (2004) 051801, arXiv:hep-ex/0402017.

[9-26]

Search for neutrino oscillations on a long base-line at the CHOOZ nuclear power station, Apollonio, M. et al. (CHOOZ), Eur. Phys. J. C27 (2003) 331, arXiv:hep-ex/0301017.
Comment: The (new) results obtained by using the prescription of Feldman and Cousins with the correct inclusion of systematics indicate that oscillations are excluded for mixing angles at high values. The limit obtained here is significantly higher than the one quoted in previous publication : ( at high values). (M.L.).

[9-27]

First Results from KamLAND: Evidence for Reactor Anti-Neutrino Disappearance, K. Eguchi et al. (KamLAND), Phys. Rev. Lett. 90 (2003) 021802, arXiv:hep-ex/0212021.
From the abstract: In an exposure of 162 tonyr (145.1 days) the ratio of the number of observed inverse -decay events to the expected number of events without disappearance is for energies 3.4 MeV. The deficit of events is inconsistent with the expected rate for standard propagation at the 99.95% confidence level. In the context of two-flavor neutrino oscillations with CPT invariance, these results exclude all oscillation solutions but the "Large Mixing Angle" solution to the solar neutrino problem using reactor sources.

[9-28]

Indications of Neutrino Oscillation in a 250 km Long- baseline Experiment, Ahn, M. H. et al. (K2K), Phys. Rev. Lett. 90 (2003) 041801, arXiv:hep-ex/0212007.
From the abstract: The K2K experiment observes indications of neutrino oscillation: a reduction of flux together with a distortion of the energy spectrum. Fifty-six beam neutrino events are observed in Super-Kamiokande (SK), 250 km from the neutrino production point, with an expectation of .
From the article: Best Fit: , .... The measured oscillation parameters are consistent with the ones suggested by atmospheric neutrinos. At the time of this letter the K2K experiment has collected approximately one-half of its planned protons on target.

[9-29]

Detection of accelerator produced neutrinos at a distance of 250-km, Ahn, S. H. et al. (K2K), Phys. Lett. B511 (2001) 178-184, arXiv:hep-ex/0103001.

[10-1]

New Results from the MINOS Experiment, Anna Holin (MINOS), arXiv:1201.3645, 2012. EPS 2011.

[10-2]

First Oscillation Results for the T2K Experiment, Mark Hartz (T2K), arXiv:1201.1846, 2012. Recontres de Moriond EW 2011.

[10-3]

New Oscillation Results from the T2K experiment, Alexander Izmaylov (T2K), arXiv:1112.0273, 2011. 15th Lomonosov Conference, August 18-24, 2011, MSU, Moscow, Russia.

[10-4]

Latest oscillation results from T2K, Marat Khabibullin (T2K), arXiv:1111.0183, 2011. New Trends in High-Energy Physics, Alushta, Crimea, Ukraine, September 3-10, 2011.

[10-5]

T2K Results and Future Plans, Francesca Di Lodovico (T2K), arXiv:1110.5382, 2011. NUFACT 11, XIIIth International Workshop on Neutrino Factories, Super beams and Beta beams, 1-6 August 2011, CERN and University of Geneva.

[10-6]

MINOS Search for Sterile Neutrinos, Alexandre Sousa (on behalf of the MINOS), arXiv:1110.3455, 2011. NUFACT 11, XIIIth International Workshop on Neutrino Factories, Superbeams and Beta beams, 1-6 August 2011, CERN and University of Geneva.

[10-7]

ICARUS and Status of Liquid Argon Technology, Dorota Stefan, arXiv:1110.1652, 2011.

[10-8]

Search for Electron Neutrino Appearance in MINOS, Mhair Orchanian (MINOS), arXiv:1109.6795, 2011. 2011 DPF.

[10-9]

Latest News from Double Chooz Reactor Neutrino Experiment, Masahiro Kuze (Double Chooz), arXiv:1109.0074, 2011. 19th Particles and Nuclei International Conference, PANIC 2011, MIT, Cambridge, MA July 2011.

[10-10]

Current status of the T2K experiment, Yuichi Oyama, on behalf of the T2K collaboration (T2K), arXiv:1108.4457, 2011. 2nd International Conference on Particle Physics (ICPP-Istanbul II),Istanbul, Turkey, June 20-25, 2011.

[10-11]

Search for oscillations in appearance mode in the OPERA experiment, Umut Kose, arXiv:1106.3871, 2011. Les Rencontres de Physique de la Vall\'ee D'Aoste (La Thuile, February 27-March 5 2011).

[10-12]

Search for oscillations in appearance mode in the OPERA experiment, L. S. Esposito (OPERA), arXiv:1105.5239, 2011. WIN'11, Cape Town, South Africa, 31 January - 5 February 2011.

[10-13]

Status of the Daya Bay Reactor Neutrino Oscillation Experiment, Cheng-Ju Lin (Daya Bay), PoS ICHEP2010 (2010) 305, arXiv:1101.0261. 35th International Conference of High Energy Physics, July 22-28, 2010, Paris, France.

[10-14]

Electron Neutrinos at T2K, Melissa George (T2K), arXiv:1006.1245, 2010.

[10-15]

The OPERA experiment: a direct search of the oscillations, J. Marteau, arXiv:0910.3468, 2009. 11th ICATPP Conference, Villa Olmo, Como, Italy, 5-9 October 2009.

[10-16]

First Observation of Accelerator Muon Antineutrinos in MINOS, Istvan Danko (MINOS), arXiv:0910.3439, 2009. DPF-2009 conference, Detroit, MI, July 27-31, 2009, eConf C090726.

[10-17]

Analysis of Neutral Current Interactions in MINOS: A Search for Sterile Neutrinos, Alexandre Sousa (MINOS), arXiv:0910.1369, 2009. DPF-2009, Detroit, MI, July 2009.

[10-18]

The OPERA experiment: on the way to the direct observation of oscillation, M. De Serio (OPERA), arXiv:0910.0337, 2009. DPF-2009, Detroit, MI, July 2009.

[10-19]

Initial Results for Electron-Neutrino Appearance in MINOS, Mayly C. Sanchez (MINOS), arXiv:0909.2362, 2009. Rencontres de Moriond EW 2009.

[10-20]

A High Precision Reactor Neutrino Detector for the Double Chooz Experiment, Fumihiko Suekane (Double Chooz), Nucl. Instrum. Meth. A623 (2010) 440-441, arXiv:0906.1639. TIPP09.

[10-21]

Status of the Double Chooz Experiment, Dawson, J. V. (Double Chooz), arXiv:0905.4843, 2009. XIII International Workshop on Neutrino Telescopes (NEUTEL09), Venice, March 10-13, 2009.

[10-22]

The OPERA experiment: Preliminary results from the 2008 run, Guillaume Lutter, arXiv:0905.4521, 2009. Lake Louise Winter Institute 2009.

[10-23]

Status Report on Double Chooz, A. Porta et al. (Double Chooz), arXiv:0905.2560, 2009. 44th Rencontres de Moriond, Electroweak interactions and unified theories, 7-14 March 2009, La Thuile.

[10-24]

Recent Results from the MINOS experiment, Milind V. Diwan, arXiv:0904.3706, 2009. XIII International Workshop on Neutrino Telescopes, March 10-13, 2009.

[10-25]

Recent Results and Future Prospects from MINOS, Jonathan M. Paley (MINOS), arXiv:0901.2131, 2009. PANIC 2008.

[10-26]

Neutrino Oscillation Studies with MINOS, Vahle, Patricia (MINOS), arXiv:0810.3627, 2008. 34th International Conference on High Energy Physics (ICHEP 2008), Philadelphia, Pennsylvania, 30 Jul - 5 Aug 2008.

[10-27]

New Results from the MINOS Experiment, Hugh Gallagher (MINOS), J. Phys. Conf. Ser. 136 (2008) 022014, arXiv:0809.5240. Neutrino 2008 Conference, Christchurch, NZ.

[10-28]

Neutrino Oscillation Results from MINOS and MiniBooNE, Tobias M. Raufer, arXiv:0808.0392, 2008. Flavor Physics and CP Violation Conference, Taipei, 2008 (FPCP 2008).

[10-29]

Current NuMI/MINOS Oscillation Results, A. Habig (MINOS), arXiv:0805.2317, 2008. Moriond Electroweak conference, March 1-8 2008.

[10-30]

Neutrino Spectra and Uncertainties for MINOS, Sacha E. Kopp (MINOS), AIP Conf. Proc. 981 (2008) 142-144, arXiv:0712.1280. NuFact07 (Okayama, Japan).

[10-31]

Preliminary Results from MINOS on Muon Neutrino Disappearance Based on an Exposure of 2.5x1020 120 GeV Protons on the NuMI Target, MINOS (MINOS), arXiv:0708.1495, 2007. XXIII International Symposium on Lepton and Photon Interactions at High Energy, Daegu Korea, August 13-18, 2007.

[10-32]

MINOS Results, Progress and Future Prospects, Tobias M. Raufer (MINOS), arXiv:0705.4655, 2007. XLIInd Rencontres de Moriond, Electroweak Interactions and Unified Theories, La Thuile, March 2007.

[10-33]

First MINOS Results with the NuMI Beam, Brian J. Rebel et al. (MINOS), Nucl. Phys. Proc. Suppl. 168 (2007) 195-198, arXiv:hep-ex/0701049. Neutrino Oscillation Workshop 2006.

[10-34]

Recent results from the MINOS experiment, Bishai, Mary (MINOS), AIP Conf. Proc. 903 (2007) 271-274.

[10-35]

The Opera Experiment, G. Giacomelli, M. Giorgini, arXiv:physics/0609045, 2006. Vulcano Workshop 2006, Frontier Objects in Astrophysics and Particle Physics, Vulcano, Italy, May 2006.

[10-36]

First MINOS Results from the NuMI Beam, Nathaniel Tagg et al. (MINOS), arXiv:hep-ex/0605058, 2006. Flavor Physics and CP Violation Conference, Vancouver, 2006.

[10-37]

Results from K2K and status of T2K, Oyama, Yuichi, arXiv:hep-ex/0512041, 2005. International Conference on New Trends in High-Energy Physics (Crimea2005), Yalta, Ukraine, September 10-17, 2005.

[10-38]

The NuMI Neutrino Beam at Fermilab, Sacha E. Kopp, arXiv:physics/0508001, 2005. U.S. Particle Accelerator Conference, Knoxville, TN (May 2005).

[10-39]

Recent Results from K2K Experiment, Mariani, C. (K2K), arXiv:hep-ex/0505019, 2005. 2005 Electroweak session, XXXXth Rencontres de Moriond.

[10-40]

HARP Experiment Results and K2K Flux, Sorel, M. (Harp), 2005. 5th International Workshop on Neutrino Beams and Instrumentation,July 7-11, 2005, Fermilab, Batavia Illinois. http://www.hep.utexas.edu/nbi2005/transparencies/beamMChadprod/sorel-HARP-results.pdf.

[10-41]

Recent K2K Results, Takanobu Ishii (K2K), arXiv:hep-ex/0406055, 2004. 5th Workshop on Neutrino Oscillations and their Origin (NOON2004), Tokyo, Japan, February 11-15,2004.

[10-42]

Recent results from K2K, Taiki Iwashita, arXiv:hep-ex/0406051, 2004. XXXIXth Rencontres de Moriond session devoted to Electroweak Interactions and Unified Theories.

[10-43]

KamLAND: updated results, Inoue, K., 2004. Neutrino Oscillation Workshop NOW 2004, September 11-17, 2004, Conca Specchiulla (Otranto, Italy). http://www.ba.infn.it/~now2004/talks/12_09_04/plen/KamLAND.pdf.

[10-44]

K2K results, T. Nakaya (K2K), 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/tuesday/nakaya.pdf.
Comment: See Recent Results From K2K.

[10-45]

Results from the KamLAND experiment, G. Gratta (KamLAND), 2004. Neutrino 2004, 13-19 June 2004, Paris, France. http://neutrino2004.in2p3.fr/slides/monday/gratta.pdf.
Comment: See Measurement of Neutrino Oscillation with KamLAND: Evidence of Spectral Distortion.

[10-46]

K2K results, Iwashita, T. (K2K), 2004. XXXIX Rencontres de Moriond, Electroweak Interactions and Unified Theories, La Thuile, 21-28 March 2003. http://moriond.in2p3.fr/EW/2004/transparencies/3_Wednesday/3_2_afternoon/3_2_4_Iwashita/Iwashita.pdf.

[10-47]

The Results of Oscillation Analysis in K2K Experiment And An Overview of JHFnu Experiment, I. Kato (K2K), arXiv:hep-ex/0306043, 2003. XXXVIIIth Recontres de Moriond on Electroweak Interaction and Unified Theories, Les Arcs, France, March 15-22, 2003.

[10-48]

Status of the Super-Kamiokande, the K2K-2 experiment and JHF nu project, Y. Hayato, 2003. EPS2003. http://eps2003.physik.rwth-aachen.de/data/talks/parallel/07Neutrino/07Hayato.ppt.

[10-49]

KamLAND Results, Inoue, K., 2003. The 4th Workshop on Neutrino Oscillations and their Origin (NOON2003), February 10-14, 2003, Ishikawa Kousei Nenkin Kaikan, Kanazawa, Japan. http://www-sk.icrr.u-tokyo.ac.jp/noon2003/transparencies/10/Inoue-KamLAND.pdf.

[10-50]

New Results from Super-K and K2K, R. Jeffrey Wilkes (K2K), eConf C020805 (2002) TTH02, arXiv:hep-ex/0212035. Secrets of the B-Meson, Topical Conference, XXX SLAC Summer Institute, SLAC, August, 2002.

[10-51]

Recent Results from the K2K Experiment, C. W. Walter (K2K), eConf C0209101 (2002) TH03, arXiv:hep-ex/0211059. Seventh International Workshop on Tau Lepton Physics (TAU02), Santa Cruz, Ca, USA, Sept 2002.

[10-52]

Present Status of the K2K Experiment, Yuichi Oyama (K2K), arXiv:hep-ex/0210030, 2002. 3rd Conference on Physics beyond the Standard Model - BEYOND THE DESERT 02 - Oulu, Finland, 2-7 June 2002. http://cupp.oulu.fi/trans/Oyama.pdf.

[10-53]

New Results from K2K, Takanobu Ishii (K2K), arXiv:hep-ex/0206033, 2002. Les Rencontres de Physique de la Vallee d'Aoste, La Thuile, Aosta Valley, Italy, March 3-9, 2002. http://www.pi.infn.it/lathuile/2002/talks/ishii.pdf.

[10-54]

An update on progress at KamLAND, Dazeley, S. A. (KamLAND), arXiv:hep-ex/0205041, 2002.

[10-55]

First Results from KamLAND: Evidence for disappearance, Gratta, G. (Kamland), 2002. SLAC Colloquium, December 2002. http://hep.stanford.edu/neutrino/KamLAND/TalksAndPublications/KamLAND_FirstResults_SLAC_Colloq.pdf.

[10-56]

KamLAND: Examination of the LMA solution with reactor neutrinos, Suzuki, A. (Kamland), 2002. XVI International Conference on Particles and Nuclei, Osaka, Japan, September 30 - October 4, 2002. http://www.rcnp.osaka-u.ac.jp/Divisions/np2/PaNic02/Suzuki.pdf.

[10-57]

K2K Results, Nishikawa, K. (K2K), 2002. XXth International Conference on Neutrino Physics and Astrophysics May 25 - 30, 2002, Munich, Germany. http://neutrino2002.ph.tum.de/pages/transparencies/nishikawa.

[11-1]

Latest Results from the MINOS Experiment, A. Blake (MINOS), 2007. TAUP 2007. http://www.awa.tohoku.ac.jp/taup2007/slides/workshop14/roomB/02-TAUP2007_MINOS.pdf.

[12-1]

Measurement of the underground atmospheric muon charge ratio using the MINOS Near Detector, P. Adamson et al. (MINOS), Phys. Rev. D83 (2011) 032011, arXiv:1012.3391.

[12-2]

Observation in the MINOS far detector of the shadowing of cosmic rays by the sun and moon, P. Adamson et al. (MINOS), Astropart. Phys. 34 (2011) 457-466, arXiv:1008.1719.

[12-3]

Zenith distribution and flux of atmospheric muons measured with the 5-line ANTARES detector, J. A. Aguilar et al. (ANTARES), Astropart. Phys. 34 (2010) 179-184, arXiv:1007.1777.

[12-4]

Measurement of the charge ratio of atmospheric muons with the CMS detector, CMS (CMS), Phys. Lett. B692 (2010) 83-104, arXiv:1005.5332.

[12-5]

Measurement of the atmospheric muon charge ratio with the OPERA detector, N. Agafonova et al. (OPERA), Eur. Phys. J. C67 (2010) 25-37, arXiv:1003.1907.

[12-6]

Measurement of the atmospheric muon flux with a 4 GeV threshold in the ANTARES neutrino telescope, J. A. Aguilar et al. (Antares), Astropart. Phys. 33 (2010) 86-90, arXiv:0910.4843.

[12-7]

Measurement of the atmospheric muon flux with the NEMO Phase-1 detector, S. Aiello et al. (The NEMO), Astropart. Phys. 33 (2010) 263-273, arXiv:0910.1269.

[12-8]

Observation of muon intensity variations by season with the MINOS far detector, Adamson, P. et al. (MINOS), Phys. Rev. D81 (2010) 012001, arXiv:0909.4012.

[12-9]

Time variations in the deep underground muon flux, S. Cecchini et al., Europhys. Lett. 87 (2009) 39001, arXiv:0907.5235.

[12-10]

Atmospheric MUons from PArametric formulas: a fast GEnerator for neutrino telescopes (MUPAGE), G. Carminati, A. Margiotta, M. Spurio, Comput. Phys. Commun. 179 (2008) 915-923, arXiv:0802.0562.

[12-11]

Study of multi-muon bundles in cosmic ray showers detected with the DELPHI detector at LEP, J. Abdallah et al. (DELPHI), Astropart. Phys. 28 (2007) 273-286, arXiv:0706.2561.

[12-12]

Measurement of the Atmospheric Muon Charge Ratio at TeV Energies with MINOS, P. Adamson et al. (MINOS), Phys. Rev. D76 (2007) 052003, arXiv:0705.3815.

[12-13]

Measurements of integral muon intensity at large zenith angles, A.N. Dmitrieva et al., arXiv:hep-ex/0611051, 2006.

[12-14]

Muon Flux at the Geographical South Pole, X. Bai et al., Astropart. Phys. 25 (2006) 361-367, arXiv:astro-ph/0602381.

[12-15]

Flux of atmospheric muons: Comparison between AIRES simulations and CAPRICE98 data, Hansen, P., Carlson, P., Mocchiutti, E., Sciutto, S. J., Boezio, M., Phys. Rev. D68 (2003) 103001, arXiv:hep-ph/0307199.

[12-16]

Measurements of Proton, Helium and Muon Spectra at Small Atmospheric Depths with the BESS Spectrometer, Abe, K. et al., Phys. Lett. B564 (2003) 8, arXiv:astro-ph/0304102.

[12-17]

Measurement of the residual energy of muons in the Gran Sasso underground Laboratories, M. Ambrosio et al. (MACRO), Astropart. Phys. 19 (2003) 313, arXiv:hep-ex/0207043.

[12-18]

Measurements of atmospheric muon spectra at mountain altitude, Sanuki, T. et al., Phys. Lett. B541 (2002) 234-242, arXiv:astro-ph/0205427.

[12-19]

Precise measurements of atmospheric muon fluxes with the BESS spectrometer, Motoki, M. et al., Astropart. Phys. 19 (2003) 113, arXiv:astro-ph/0205344.

[12-20]

Measurement of the flux of atmospheric muons with the CAPRICE94 apparatus, Boezio, M. et al. (WiZard/CAPRICE), Phys. Rev. D62 (2000) 032007, arXiv:hep-ex/0004014.

[12-21]

Energy spectra, altitude profiles and charge ratios of atmospheric muons, Coutu, S. et al., Phys. Rev. D62 (2000) 032001, arXiv:hep-ex/0004010.

[12-22]

Balloon measurements of cosmic ray muon spectra in the atmosphere along with those of primary protons and helium nuclei over mid-latitude, Bellotti, R. et al. (WiZard/MASS2), Phys. Rev. D60 (1999) 052002, arXiv:hep-ex/9905012.

[12-23]

A Measurement of the negative muon spectrum between 0.3- GeV/c and 40-GeV/c in the atmosphere, Bellotti, R. et al., Phys. Rev. D53 (1996) 35-43.

[12-24]

Zenith-angle dependence of cosmic ray muons, Bergeson, H. E. et al., Phys. Rev. Lett. 27 (1971) 160-163.

[12-25]

Cosmic ray muon intensity deep underground versus depth, Meyer, B. S. et al., Phys. Rev. D1 (1970) 2229-2244.

[13-1]

Observations of Large Scale Sidereal Anisotropy in 1 and 11 TeV cosmic rays from the MINOS experiment, J.K. de Jong (MINOS), arXiv:1201.2621, 2012. 32nd International Cosmic Ray Conference, August 2011.

[13-2]

Measurement of the atmospheric muon flux with the ANTARES detector, Marco Bazzotti et al. (ANTARES), arXiv:0911.3055, 2009. 31st ICRC, Lodz 2009.

[13-3]

Direct Measurement of the Atmospheric Muon Energy Spectrum with IceCube, Patrick Berghaus (IceCube), arXiv:0909.0679, 2009. 31st ICRC, Lodz, Poland, July 2009.

[13-4]

Large Scale Cosmic Ray Anisotropy With IceCube, Abbasi, Rasha, Desiati, Paolo, Collaboration, for the IceCube, Astrophys. J. 718 (2010) L194, arXiv:0907.0498. ICRC (2009).

[13-5]

MINOS Observations of Shadowing in the Muon Flux Underground, Grashorn, E. W. (MINOS), arXiv:0710.1617, 2007. 30th International Cosmic Ray Conference (ICRC 2007), Merida, Yucatan, Mexico, 3-11 Jul 2007.

[13-6]

Observation of Seasonal Variations with the MINOS Far Detector, E.W. Grashorn (MINOS), arXiv:0710.1616, 2007. 30th International Cosmic Ray Conference (ICRC 2007), Merida, Yucatan, Mexico, 3-11 Jul 2007.

[13-7]

The Maximum Detectable Momentum for cosmic ray muons in the MINOS far detector, Maury Goodman (MINOS), arXiv:0706.0539, 2007. 30th International Cosmic Ray Conference, Merida Mexico 2007.

[13-8]

Interpretation of the atmospheric muon charge ratio in MINOS, Philip Schreiner, Maury Goodman (MINOS), arXiv:0706.0538, 2007. 30th International Cosmic Ray Conference, Merida Mexico 2007.

[13-9]

Measurement of the atmospheric muon spectrum from 20 to 2000 GeV, Michael Unger et al. (L3), eConf C030626 (2003) FRAP03, arXiv:hep-ex/0309002. XXIII Physics in Collisions Conference (PIC03), Zeuthen, Germany, June 2003.

[14-1]

Atmospheric gamma-ray observation with the BETS detector for calibrating atmospheric neutrino flux calculations, Kasahara, K. et al., Phys. Rev. D66 (2002) 052004, arXiv:hep-ex/0206055.
From the article: The observed gamma-ray fluxes are compared with calculations employed by the HKKM group [15-42] wich were used in comparison with the Kamioka neutrino data. It is found that the interaction model used in the HKKM calculations is not a very good model.

[15-1]

Improvement of low energy atmospheric neutrino flux calculation using the JAM nuclear interaction model, Morihiro Honda, Takaaki Kajita, Katsuaki Kasahara, Shoichi Midorikawa, Phys. Rev. D83 (2011) 123001, arXiv:1102.2688.

[15-2]

Atmospheric lepton fluxes at very high energy, J.I. Illana, Paolo Lipari, M. Masip, D. Meloni, Astropart. Phys. 34 (2011) 663-673, arXiv:1010.5084.

[15-3]

Atmospheric lepton fluxes at ultrahigh energies, J.I. Illana, M. Masip, D. Meloni, JCAP 0909 (2009) 008, arXiv:0907.1412.

[15-4]

Prompt neutrino fluxes from atmospheric charm, Rikard Enberg, Mary Hall Reno, Ina Sarcevic, Phys. Rev. D78 (2008) 043005, arXiv:0806.0418.

[15-5]

Calculation of atmospheric neutrino flux using the interaction model calibrated with atmospheric muon data, M. Honda et al., Phys. Rev. D75 (2007) 043006, arXiv:astro-ph/0611418.

[15-6]

Uncertainties in Atmospheric Neutrino Fluxes, G.D. Barr, T.K. Gaisser, S. Robbins, T. Stanev, Phys. Rev. D74 (2006) 094009, arXiv:astro-ph/0611266.

[15-7]

Study of cosmic ray interaction model based on atmospheric muons for the neutrino flux calculation, T. Sanuki et al., Phys. Rev. D75 (2007) 043005, arXiv:astro-ph/0611201.

[15-8]

Simulation of neutrino and charged particle production and propagation in the atmosphere, L. Derome, Phys. Rev. D74 (2006) 105002, arXiv:astro-ph/0607619.

[15-9]

A semi-analytic calculation on the atmospheric tau neutrino flux due to oscillations, Fei-Fan Lee, Guey-Lin Lin, Astropart. Phys. 25 (2006) 64, arXiv:hep-ph/0412383.

[15-10]

Fluxes of Atmospheric Leptons at 600 GeV - 60 TeV, Dmitry Chirkin, arXiv:hep-ph/0407078, 2004.

[15-11]

A New calculation of the atmospheric neutrino flux in a 3-dimensional scheme, M.Honda, T.Kajita, K.Kasahara, S.Midorikawa, Phys. Rev. D70 (2004) 043008, arXiv:astro-ph/0404457.
From the abstract: We estimate the total uncertainty of the atmospheric neutrino flux prediction is reduced to below 10 GeV.... The uncertainty of the absolute normalization of the atmospheric neutrino is still large above 10 GeV due to the uncertainty of the primary cosmic ray flux above 100 GeV. However, the zenith angle variation is not affected by these uncertainties.

[15-12]

A three-dimensional calculation of atmospheric neutrinos, G.D. Barr et al., Phys. Rev. D70 (2004) 023006, arXiv:astro-ph/0403630.
From the article: We have extended the 1-dimensional neutrino flux calculation~[15-49,] to three dimensions. We compare results of the 3D and 1D calculations for neutrino energies from 100 MeV to 10 GeV over the full solid angle. Results are given for Kamioka, which is at low geomagnetic latitude, and for SNO and Soudan at high latitude.
The angle-averaged fluxes are identical within statistics for ~GeV, with approximately a 3% excess in the 3D calculation for sub-GeV neutrinos. The differences are much more noticeable in the zenith angle distributions for ~GeV, which show a significant excess in the 3D calculation for and a smaller deficit for . The differences largely cancel in the angular integral, leaving the small (3%) overall difference mentioned above. The zenith-angle differences decrease with energy and become completely negligible for ~GeV.
Corresponding to the horizontal excess in the 3D calculation is a contribution to the path length distribution of near horizontal neutrinos which reduces the average path length for horizontal neutrinos with ~MeV by 15% relative to the 1D calculation. The corresponding reduction decreases to 4% for ~GeV.

[15-13]

A 3-d simulation of the atmospheric neutrinos, Favier, J., Kossakowski, R., Vialle, J. P, Phys. Rev. D68 (2003) 093006, arXiv:astro-ph/0305460.

[15-14]

Calculation of fluxes of charged particles and neutrinos from atmospheric showers, Plyaskin, V., arXiv:hep-ph/0303146, 2003.

[15-15]

Prompt neutrinos from atmospheric c-cbar and b-bbar production and the gluon at very small x, A.D. Martin, M.G. Ryskin, A.M. Stasto, Acta Phys. Polon. B34 (2003) 3273, arXiv:hep-ph/0302140.

[15-16]

Simulation of Atmospheric Muon and Neutrino Fluxes with CORSIKA, Wentz, J. et al., Phys. Rev. D67 (2003) 073020, arXiv:hep-ph/0301199.
Comment: Comparisons at the Kamioka site between CORSIKA and FLUKA vertical neutrino fluxes are given in corsika.pdf (courtesy of G. Battistoni).

[15-17]

Atmospheric neutrino flux from 3-dimensional simulation, Liu, Yong, Derome, L., Buenerd, M., Phys. Rev. D67 (2003) 073022, arXiv:astro-ph/0211632.
From the abstract: The flux obtained at the Super-Kamiokande experiment location are reported and compared with other calculations. For low neutrino energies the flux obtained is significantly smaller than that used in the data analysis of underground experiment.

[15-18]

The FLUKA atmospheric neutrino flux calculation, Battistoni, G., Ferrari, A., Montaruli, T., Sala, P. R., Astropart. Phys. 19 (2003) 269, arXiv:hep-ph/0207035.
Comment: Fig. 17 and Fig. 18 give a crude comparison between the new FLUKA-3D calculation at the Super-Kamiokande site and the old neutrino flux calculations of Ref. [] and [15-42] that have been used extensively as input to the detector simulation. The new absolute flux normalization is clearly lower. (M.L.).

[15-19]

Comparison of the FLUKA calculations with CAPRICE94 data on muons in atmosphere, Battistoni, G., Ferrari, A., Montaruli, T., Sala, P. R., Astropart. Phys. 17 (2002) 477-488, arXiv:hep-ph/0107241.

[15-20]

Semi-analytic approximations for production of atmospheric muons and neutrinos, Gaisser, Thomas K., Astropart. Phys. 16 (2002) 285-294, arXiv:astro-ph/0104327.

[15-21]

Comparison of 3-dimensional and 1-dimensional schemes in the calculation of atmospheric neutrinos, Honda, M., Kajita, T., Kasahara, K., Midorikawa, S., Phys. Rev. D64 (2001) 053011, arXiv:hep-ph/0103328.

[15-22]

Atmospheric neutrino flux supported by recent muon experiments, Fiorentini, Giovanni, Naumov, Vadim A., Villante, Francesco L., Phys. Lett. B510 (2001) 173-188, arXiv:hep-ph/0103322.
From the abstract: A comparison with the muon fluxes and charge ratios measured in several modern balloon-borne experiments suggests that the atmospheric neutrino flux is essentially lower than one used for the standard analyses of the sub-GeV and multi-Gev neutrino induced events in underground detectors.

[15-23]

Calculation of atmospheric neutrino flux, Plyaskin, Vassily (AMS), Phys. Lett. B516 (2001) 213-235, arXiv:hep-ph/0103286.
From the article: The simulation correctly describes the fluxes of protons and leptons () measured by AMS. The results of our Monte Carlo study of propagation in space and interaction with the atmosphere of cosmic particle show that the primary proton flux in the vicinity of the Earth is essentially anisotropic at the directions approaching the horizontal plane. The horizontal region is the most important for determination of the up/down asymmetry of the atmospheric neutrino fluxes and consequently the result of the present study may affect the eventual experimental measurement of the neutrino oscillation parameter . The atmospheric neutrinos produced in our simulation have the energy spectra, relative fluxes and angular distributions different from those obtained in the previous atmospheric flux calculations.

[15-24]

The fluxes of sub-cutoff particles detected by AMS, the cosmic ray albedo and atmospheric neutrinos, Lipari, Paolo, Astropart. Phys. 16 (2002) 295-323, arXiv:astro-ph/0101559.

[15-25]

Fluxes of cosmic ray muons and atmospheric neutrinos at high energies, Volkova, L. V., Zatsepin, G. T., Phys. Atom. Nucl. 64 (2001) 266-274.

[15-26]

The east-west effect for atmospheric neutrinos, Lipari, Paolo, Astropart. Phys. 14 (2000) 171-188, arXiv:hep-ph/0003013.

[15-27]

The geometry of atmospheric neutrino production, Lipari, Paolo, Astropart. Phys. 14 (2000) 153-170, arXiv:hep-ph/0002282.

[15-28]

Primary cosmic rays, antiprotons and atmospheric neutrinos, Gaisser, T. K., Phys. Scripta T85 (2000) 100-105.

[15-29]

A three-dimensional calculation of atmospheric neutrino fluxes, Tserkovnyak, Yaroslav, Komar, Robert, Nally, Christian, Waltham, Chris, Astropart. Phys. 18 (2003) 449, arXiv:hep-ph/9907450.

[15-30]

A 3-dimensional calculation of atmospheric neutrino flux, Battistoni, G. et al., Astropart. Phys. 12 (2000) 315-333, arXiv:hep-ph/9907408.

[15-31]

Uncertainties in prompt atmospheric neutrino flux calculations, Volkova, L. V., Zatsepin, G. T., Phys. Lett. B462 (1999) 211-216.

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Atmospheric muon flux at sea level, underground and underwater, Bugaev, E. V. et al., Phys. Rev. D58 (1998) 054001, arXiv:hep-ph/9803488.

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Geomagnetic effects on atmospheric neutrinos, Lipari, Paolo, Stanev, Todor, Gaisser, T. K., Phys. Rev. D58 (1998) 073003, arXiv:astro-ph/9803093.

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The K(l3) form factors and atmospheric neutrino flavor ratio at high energies, Naumov, V. A., Sinegovskaya, T. S., Sinegovsky, S. I., Nuovo Cim. A111 (1998) 129-148, arXiv:hep-ph/9802410.

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New calculation of atmospheric neutrino fluxes, Mitsui, K., Minorikawa, Y., Takazawa, M., Nuovo Cim. C21 (1998) 99-112.

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[15-41]

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[15-42]

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[15-43]

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[15-44]

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[15-45]

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[16-1]

High-energy spectrum and zenith-angle distribution of atmospheric neutrinos, S. I. Sinegovsky, O. N. Petrova, T. S. Sinegovskaya, arXiv:1109.3576, 2011. 32nd ICRC (Beijing, China, 11-18 Aug. 2011).

[16-2]

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Comment: Slide n.10 gives the comparison between Superkamiokande atmospheric neutrino data (Sub-Gev and Multi-GeV samples as a function of zenith angle) and various MC neutrino flux calculations. In green FLUKA, in blue the NEW HONDA, in red the OLD HONDA. The comparison is taken from M.Shiozawa's Review on experimental results on cosmic ray neutrinos - AMS collaboration meeting - October 2001 - Trento - Italy. In the case of FLUKA MC calculation an excess of electron-like data events is clearly visible in both the Sub-GeV and the Multi-GeV samples. (M.L.).

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Three-neutrino model analysis of the world's oscillation data, D. C. Latimer, D. J. Ernst, arXiv:nucl-th/0310083, 2003.
Comment: Another junk paper in which it is claimed that solar, atmospheric and LSND data can be fitted in a three-neutrino model.
Important data (energy spectra) are omitted and the analysis is very approximate.
The claimed best-fit values of the largest are either or .
The smaller value give in LSND. Therefore, this case is equivalent to neglect LSND.
The larger values obviously cannot fit the energy spectra of atmospheric neutrinos, which have been omitted in the analysis.
[C.G.].

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Atmospheric neutrinos: LMA oscillations, Ue3 induced interference and CP-violation, O. L. G. Peres, A. Yu. Smirnov, Nucl. Phys. B680 (2004) 479, arXiv:hep-ph/0309312.

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From the article: ... we conclude that due to the uncertainty of the identification capability for muon and electron events in Super K. detector one cannot yet firmly establish the existence of an atmospheric neutrino anomaly.

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From the abstract: ... all four-neutrino descriptions of the LSND anomaly, both in (2+2) as well as (3+1) realizations, are highly disfavoured. Our analysis brings the LSND hint to a more puzzling status.
From the article: The exclusion of four-neutrino oscillation schemes of the (2+2)-type is based on the improved sensitivity of solar and atmospheric neutrino experiments to oscillations into a sterile neutrino, thanks to recent experimental data. This is a very robust result, independent of whether the LSND experiment is confirmed or disproved. The exclusion of (3+1) schemes depends somehow on the used LSND data. Furthermore, it heavily relies on the results of negative SBL experiments, especially on the Bugey and CDHS disappearance experiments.

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