Measurement of the atmospheric muon spectrum from 20 to 3000 GeV

Achard, P.; Адриани, О.; Aguilar-Benı́tez, M.; Akker, M. van den; Alcaraz, J.; Alemanni, G.; Allaby, J.; Aloisio, A.; Alviggi, M. G.; Anderhub, H.; Andreev, V.; Anselmo, F.; Arefiev, A.; Azemoon, T.; Aziz, T.; Bagnaia, P.; Bajo, A.; Baksay, G.; Baksay, L.; Bähr, J.; Baldew, S.V.; Banerjee, S.; Barczyk, A.; Barillère, R.; Bartalini, P.; Basile, M.; Batalova, N.; Battiston, R.; Bay, A.; Becattini, F.; Becker, U.; Behner, F.; Bellucci, L.; Berbeco, R.; Berdugo, J.; Berges, P.; Bertucci, B.; Betev, B. L.; Biasini, M.; Biglietti, M.; Biland, A.; Blaising, J. J.; Blyth, S.; Bobbink, G. J.; Böhm, A.; Boldizsár, L.; Borgia, B.; Bottai, S.; Bourilkov, D.; Bourquin, M.; Braccini, S.; Branson, J. G.; Brochu, F. M.; Burger, J. D.; Burger, W. J.; Cai, X.; Capell, M.; Romeo, G. Cara; Carlino, G.; Cartacci, A. M.; Casaus, J.; Cavallari, F.; Cavallo, N.; Cecchi, C.; Cerrada, M.; Chamizo, M.; Chiarusi, T.; Chang, Y. H.; Chemarin, M.; Chen, A.; Chen, G.; Chen, G.M.; Chen, H.F.; Chen, H.S.; Chiefari, G.; Cifarelli, L.; Cindolo, F.; Clare, I.; Clare, R.; Coignet, G.; Colino, N.; Costantini, S.; Cruz, B. De La; Cucciarelli, S.; Dalen, J. A. van; Asmundis, R. de; Déglon, P.; Debreczeni, J.; Degré, A.; Dehmelt, K.; Deiters, K.; Volpe, D. della; Delmeire, E.; Denes, P.; DeNotaristefani, F.; Salvo, A. De; Diemoz, M.; Dierckxsens, M.; Ding, L. K.; Dionisi, C.; Dittmar, M.; Doria, A.; Dova, M. T.; Duchesneau, D.; Duda, M.; Durán, I.; Echenard, B.; Eline, A.; Hage, A. El; Mamouni, H. El; Engler, A.; Eppling, F. J.; Extermann, P.; Faber, G.; Falagán, M. A.; Falciano, S.; Favara, A.; Fay, J.; Fedin, O. L.; Felcini, M.; Ferguson, T.; Fesefeldt, H.; Fiandrini, E.; Field, J. H.; Filthaut, F.; Fisher, W. C.; Fisk, I.; Forconì, G.; Freudenreich, K.; Furetta, C.; Galaktionov, Yu.; Ganguli, S. N.; Garcı́a-Abia, P.; Gataullin, M.; Gentile, S.; Giagu, S.; Gong, Z. F.; Grabosch, H. J.; Grenier, G.; Grimm, O.; Groenstege, H.; Gruenewald, M. W.; Guida, M.; Guo, Y.N.; Gupta, S. K.; Gupta, V. K.; Gurtu, A.; Gutay, L.; Haas, D.; Haller, C.; Hatzifotiadou, D.; Hayashi, Y.; He, Zhi-Guo; Hebbeker, T.; Hervé, A.; Hirschfelder, J.; Höfer, H.; Hohlmann, M.; Holzner, G.; Hou, S.; Huo, A. X.; Hu, Yiming; Ito, N.; Jin, B. N.; Jing, C. L.; Jones, L. W.; Jong, P. de; Josa-Mutuberrı́a, I.; Kantserov, V. A.; Kaur, M.; Kawakami, S.; Kienzle‐Focacci, M. N.; Kim, J.K.; Kirkby, J.; Kittel, W.; Klimentov, A.; König, A. C.; Kok, E.; Korn, A.; Kopál, M.; Koutsenko, V.; Kräber, M.; Kuang, H.H.; Kraemer, R.W.; Krüger, A.; Kuijpers, J.; Kunin, A.; Guevara, P. Ladrón de; Laktineh, I. B.; Landi, G.; Lebeau, M.; Lebedev, A.; Lebrun, P.; Lecomte, P.; Lecoq, P.; Coultre, P. Le; Goff, J. M. Le; Lei, Y. J.; Leich, H.; Leiste, R.; Levtchenko, M.; Levtchenko, P.; Li, C.; Li, L.; Li, Z.C.; Likhoded, S.; Lin, C. H.; Lin, W.; Linde, F.L.; Lista, L.; Liu, Z.A.; Lohmann, W.; Longo, E.; Lu, Y.S.; Luci, C.; Luminari, L.; Lustermann, W.; Ma, W.G.; Ma, Xiaohua; Ma, Yuqian; Malgeri, L.; Малинин, А.; Mañá, C.; Mans, J.; Martin, J. P.; Marzano, F.; Mazumdar, K.; McNeil, R. R.; Mele, S.; Meng, X.; Merola, L.; Meschini, M.; Metzger, W. J.; Mihul, A.; Mil, A. van; Milcent, H.; Mirabelli, G.; Mnich, J.; Mohanty, G. B.; Monteleoni, B.; Muanza, G. S.; Muijs, A. J.M.; Musicar, B.; Musy, M.; Nagy, S.; Nahnhauer, R.; Naumov, Vadim A.; Natale, Sonia; Napolitano, M.; Nessi‐Tedaldi, F.; Newman, H. B.; Nisati, A.; Novák, T.; Nowak, H.; Ofierzynski, R. A.; Organtini, G.; Pal, I.; Palomares, C.; Paolucci, P.; Paramatti, R.; Parriaud, J.-F.; Passaleva, G.; Patricelli, S.; Paul, T.; Pauluzzi, M.; Paus, C.; Pauß, F.; Pedace, M.; Pensotti, S.; Perret-Gallix, D.; Petersen, B.; Piccolo, D.; Pierella, F.; Pieri, M.; Pioppí, M.; Piroué, P.; Pistolesi, E.; Plyaskin, V.; Pohl, M.; Pojidaev, V.; Pothier, J.; Prokofiev, D.; Quartieri, J.; Cheng-Rui, Qing; Rahal-Callot, G.; Rahaman, M. A.; Raics, P.; Raja, N.; Ramelli, R.; Rancoita, P.G.; Ranieri, R.; Raspereza, A.; Ravindran, K.; Razis, P. A.; Ren, D.; Rescigno, M.; Reucroft, S.; Rewiersma, P.; Riemann, S.; Riles, K.; Roe, B.P.; Rojkov, A.; Romero, L.; Rosca, A.; Rosemann, C.; Rosenbleck, C.; Rosier‐Lees, S.; Roth, Stefan; Rubio, J. A.; Ruggiero, G.; Rykaczewski, H.; Saidi, R.; Sakharov, A.; Saremi, S.; Sarkar, S.; Salicio, J.; Sánchez, E.; Schäfer, Christian; Schegelsky, V. A.; Schmitt, V.; Schoeneich, B.; Schopper, H.; Schotanus, D. J.; Sciacca, C.; Servoli, L.; Shen, C.; Shevchenko, S.; Shivarov, N.; Shoutko, V.; Shumilov, E.; Shvorob, A.; Son, D.; Souga, C.; Спиллантини, П.; Steuer, M.; Stickland, D.; Stoyanov, B.; Straessner, A.; Sudhakar, K.; Sulanke, H.; Sultanov, G.; Sun, L.; Sushkov, S.; Suter, H.; Swain, J.; Szillási, Z.; Tang, X. W.; Tarján, P.; Tauscher, L.; Taylor, L.; Tellili, B.; Teyssier, D.; Timmermans, C.; Ting, Samuel C.C.; Ting, S. M.; Tonwar, S. C.; Töth, J.; Trowitzsch, G.; Tully, C.; Tung, K. L.; Ulbricht, J.; Unger, Michael; Valente, E.; Verkooijen, H.; Walle, R. T. Van de; Vasquez, Raymond; Veszprémi, V.; Vesztergombi, G.; Vetlitsky, I.; Vicinanza, D.; Viertel, G.; Villa, S.; Vivargent, M.; Vlachos, S.; Vodopianov, I.; Vogel, H.; Vogt, H.; Vorobiev, I.; Vorobyov, A.A.; Wadhwa, M.; Wang, R.G.; Wang, Q.; Wang, X.L.; Wang, X.W.; Wang, Z.M.; Weber, Martin; Wijk, R. van; Wijnen, T.; Wilkens, H. G.; Wynhoff, S.; Xia, L.; Xu, Yupeng; Xu, J.; Xu, Z.; Yamamoto, J.; Yang, B. Z.; Yang, C.; Yang, Hai; Yang, M. T.; Yang, Xinzheng; Yao, Z. G.; Yeh, Sc; Yu, Zhao-Huan; Zalite, A.; Zalite, Yu; Zhang, C.; Zhang, F.; Zhang, J.; Zhang, S.; Zhang, Z.P.; Zhao, Junjie; Zhou, S.; Zhu, G. Y.; Zhu, R. Y.; Zhuang, H.L.; Zhu, Q. Q.; Zichichi, A.; Zimmermann, B.; Zöller, Margot; Zwart, A.

doi:10.1016/j.physletb.2004.08.003

Cited by 111 publications

(68 citation statements)

References 36 publications

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“…The method has therefore large systematic uncertainties. L3 + C has recently measured precisely the muon momentum spectrum, as well as the charge ratio and the angular dependence [16]. Based on to-dayÕs knowledge of the parameters entering the calculation, an estimate of an upper limit on the contribution of antiprotons to the primary flux could not compete with the one presented in this paper.…”

Section: Cosmic-ray Antiprotonsmentioning

confidence: 89%

Measurement of the shadowing of high-energy cosmic rays by the Moon: A search for TeV-energy antiprotons

Achard

Адриани

Akker

et al. 2005

Astroparticle Physics

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The shadowing of high-energy cosmic rays by the Moon has been observed with a significance of 9.4 standard deviations with the L3 + C muon spectrometer at CERN. A significant effect of the Earth magnetic field is observed. Since 6 Supported by the German Bundesministerium fü r Bildung, Wissenschaft, Forschung und Technologie. 7 Supported by the Hungarian OTKA fund under contract numbers T019181, F023259 and T037350. 8 Supported by the National Natural Science Foundation of China. 9 Also supported by the Hungarian OTKA fund under contract number T026178. no event deficit on the east side of the Moon has been observed, an upper limit at 90% confidence level on the antiproton to proton ratio of 0.11 is obtained for primary energies around 1 TeV.

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Section: Cosmic-ray Antiprotonsmentioning

confidence: 89%

Measurement of the shadowing of high-energy cosmic rays by the Moon: A search for TeV-energy antiprotons

Achard

Адриани

Akker

et al. 2005

Astroparticle Physics

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“…We include the conventional µ + + µ − , ν µ + ν µ and ν e + ν e fluxes (from the vertical direction) taking into account only the decay of charged pions and kaons. The data points are from the L3 detector [12]. Inspection of Fig.…”

Section: Atmospheric Muons From Unflavored Mesonsmentioning

confidence: 99%

Atmospheric muon and neutrino fluxes at very high energy

Illana¹,

Lipari²,

Masip³

et al. 2011

Astroparticle Physics

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The observation of astrophysical neutrinos requires a detailed understanding of the atmospheric neutrino background. Since neutrinos are produced in meson decays together with a charged lepton, important constraints on this background can be obtained from the measurement of the atmospheric muon flux. Muons, however, can also be produced as µ + µ − pairs by purely electromagnetic processes. We use the Z-moment method to study and compare the contributions to the atmospheric muon and neutrino fluxes from different sources (π/K decay, charmed and unflavored hadron decay, and photon conversion into a muon pair). We pay special attention to the contribution from unflavored mesons (η, η , ρ • , ω and φ). These mesons are abundant in air showers, their lifetimes are much shorter than those of charged pions or kaons, and they have decay branching ratios of order 10 −4 into final states containing a muon pair. We show that they may be the dominant source of muons at E µ 10 3 TeV.

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“…This verification may be carried out by comparing model predictions of this muon fluxes with data. We select the classical experiments L3+Cosmic [15], MACRO [16] and LVD [17] and elaborate the smooth approximation of these muon data in the energy interval of 10 2 − 10 5 GeV. The model predictions of muon flux have been estimate as follows.…”

Section: Introductionmentioning

confidence: 99%

“…A comparison of muon data observed in [15][16][17] with results of simulations allows to draw a conclusion about the most energetic mesons production described by these models.…”

Section: Introductionmentioning

confidence: 99%

Testing of the VENUS 4.12, DPMJET 2.55, QGSJET II-03 and SIBYLL 2.3 hadronic interaction models via help of the atmospheric vertical muon spectra

et al. 2017

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Abstract.Uncertainties of the model energy spectra of the most energetic secondary π ± -mesons (and K ± -mesons) are discussed. Computer simulations of the partial energy spectra of the atmospheric vertical muons induced by primary cosmic particles with various fixed energies in interval 10 2 −10 7 GeV in terms of the VENUS 4.12, DPMJET 2.55, QGSJET II-03 and SIBYLL 2.3 models had been carried out with help of CORSIKA package. These partial spectra should be convoluted with the contemporary spectra of the primary cosmic particles. Results of simulations are compared with the contemporary atmospheric vertical muon flux data. Comparison shows that all models underestimate production of secondary π ± -mesons (and K ± -mesons) by factor of ∼ 2 at the most high energies. This underestimation induces more rapid development of extensive air showers in the atmosphere and results in uncertainties in estimates of energy and composition of the primary cosmic particles.

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Measurement of the atmospheric muon spectrum from 20 to 3000 GeV

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Cited by 111 publications

References 36 publications

Measurement of the shadowing of high-energy cosmic rays by the Moon: A search for TeV-energy antiprotons

Measurement of the shadowing of high-energy cosmic rays by the Moon: A search for TeV-energy antiprotons

Atmospheric muon and neutrino fluxes at very high energy

Testing of the VENUS 4.12, DPMJET 2.55, QGSJET II-03 and SIBYLL 2.3 hadronic interaction models via help of the atmospheric vertical muon spectra

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