Measurement of the TeV atmospheric muon charge ratio with the complete OPERA data set

N. Agafonova; A. Aleksandrov; A. Anokhina; S. Aoki; A. Ariga; T. Ariga; D. Bender; A. Bertolin; C. Bozza; R. Brugnera; A. Buonaura; S. Buontempo; B. Büttner; M. Chernyavsky; A. Chukanov; L. Consiglio; N. D'Ambrosio; G. De Lellis; M. De Serio; P. Del Amo Sanchez; A. Di Crescenzo; D. Di Ferdinando; N. Di Marco; S. Dmitrievski; M. Dracos; D. Duchesneau; S. Dusini; T. Dzhatdoev; J. Ebert; A. Ereditato; R. A. Fini; T. Fukuda; G. Galati; A. Garfagnini; G. Giacomelli; C. Göllnitz; J. Goldberg; Y. Gornushkin; G. Grella; M. Guler; C. Gustavino; C. Hagner; T. Hara; A. Hollnagel; B. Hosseini; H. Ishida; K. Ishiguro; K. Jakovcic; C. Jollet; C. Kamiscioglu; M. Kamiscioglu; J. Kawada; J. H. Kim; S. H. Kim; N. Kitagawa; B. Klicek; K. Kodama; M. Komatsu; U. Kose; I. Kreslo; A. Lauria; J. Lenkeit; A. Ljubicic; A. Longhin; P. Loverre; A. Malgin; M. Malenica; G. Mandrioli; T. Matsuo; V. Matveev; N. Mauri; E. Medinaceli; A. Meregaglia; S. Mikado; P. Monacelli; M. C. Montesi; K. Morishima; M. T. Muciaccia; N. Naganawa; T. Naka; M. Nakamura; T. Nakano; Y. Nakatsuka; K. Niwa; S. Ogawa; N. Okateva; A. Olshevsky; T. Omura; K. Ozaki; A. Paoloni; B. D. Park; I. G. Park; L. Pasqualini; A. Pastore; L. Patrizii; H. Pessard; C. Pistillo; D. Podgrudkov; N. Polukhina; M. Pozzato; F. Pupilli; M. Roda; H. Rokujo; T. Roganova; G. Rosa; O. Ryazhskaya; O. Sato; A. Schembri; I. Shakiryanova; T. Shchedrina; A. Sheshukov; H. Shibuya; T. Shiraishi; G. Shoziyoev; S. Simone; M. Sioli; C. Sirignano; G. Sirri; M. Spinetti; L. Stanco; N. Starkov; S. M. Stellacci; M. Stipcevic; P. Strolin; S. Takahashi; M. Tenti; F. Terranova; V. Tioukov; S. Tufanli; P. Vilain; M. Vladimirov; L. Votano; J. L. Vuilleumier; G. Wilquet; B. Wonsak; C. S. Yoon; S. Zemskova; A. Zghiche

doi:10.1140/epjc/s10052-014-2933-0

Measurement of the TeV atmospheric muon charge ratio with the complete OPERA data set

N. Agafonova, A. Aleksandrov, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, D. Bender, A. Bertolin, C. Bozza, R. Brugnera, A. Buonaura, S. Buontempo, B. Büttner, M. Chernyavsky, A. Chukanov, L. Consiglio, N. D'Ambrosio, G. De Lellis, M. De Serio, P. Del Amo SanchezA. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievski, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, R. A. Fini, T. Fukuda, G. Galati, A. Garfagnini, G. Giacomelli, C. Göllnitz, J. Goldberg, Y. Gornushkin, G. Grella, M. Guler, C. Gustavino, C. Hagner, T. Hara, A. Hollnagel, B. Hosseini, H. Ishida, K. Ishiguro, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, J. Kawada, J. H. Kim, S. H. Kim, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, A. Lauria, J. Lenkeit, A. Ljubicic, A. Longhin, P. Loverre, A. Malgin, M. Malenica, G. Mandrioli, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, S. Mikado, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, Y. Nakatsuka, K. Niwa, S. Ogawa, N. Okateva, A. Olshevsky, T. Omura, K. Ozaki, A. Paoloni, B. D. Park, I. G. Park, L. Pasqualini, A. Pastore, L. Patrizii, H. Pessard, C. Pistillo, D. Podgrudkov, N. Polukhina, M. Pozzato, F. Pupilli, M. Roda, H. Rokujo, T. Roganova, G. Rosa, O. Ryazhskaya, O. Sato, A. Schembri, I. Shakiryanova, T. Shchedrina, A. Sheshukov, H. Shibuya, T. Shiraishi, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, P. Strolin, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, S. Tufanli, P. Vilain, M. Vladimirov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, C. S. Yoon, S. Zemskova, A. Zghiche

Research output: Contribution to journal › Article › peer-review

33 Citations (Scopus)

Abstract

The OPERA detector, designed to search for νμ → ντ oscillations in the CNGS beam, is located in the underground Gran Sasso laboratory, a privileged location to study TeV-scale cosmic rays. For the analysis here presented, the detector was used to measure the atmospheric muon charge ratio in the TeV region. OPERA collected chargeseparated cosmic ray data between 2008 and 2012. More than 3 million atmospheric muon events were detected and reconstructed, among which about 110000 multiple muon bundles. The charge ratio R_μ ≡ N_μ+/N_μ − was measured separately for single and for multiple muon events. The analysis exploited the inversion of the magnet polarity which was performed on purpose during the 2012 Run. The combination of the two data sets with opposite magnet polarities allowedminimizing systematic uncertainties and reaching an accurate determination of the muon charge ratio. Data were fitted to obtain relevant parameters on the composition of primary cosmic rays and the associated kaon production in the forward fragmentation region. In the surface energy range 1–20 TeV investigated by OPERA, R_μ is well described by a parametric model including only pion and kaon contributions to themuon flux, showing no significant contribution of the prompt component. The energy independence supports the validity of Feynman scaling in the fragmentation region up to 200 TeV/nucleon primary energy.

Original language	English
Article number	2933
Pages (from-to)	1-9
Number of pages	9
Journal	European Physical Journal C
Volume	74
Issue number	7
DOIs	https://doi.org/10.1140/epjc/s10052-014-2933-0
Publication status	Published - Jul 15 2014
Externally published	Yes

All Science Journal Classification (ASJC) codes

Engineering (miscellaneous)
Physics and Astronomy (miscellaneous)

Access to Document

10.1140/epjc/s10052-014-2933-0

Cite this

Agafonova, N., Aleksandrov, A., Anokhina, A., Aoki, S., Ariga, A., Ariga, T., Bender, D., Bertolin, A., Bozza, C., Brugnera, R., Buonaura, A., Buontempo, S., Büttner, B., Chernyavsky, M., Chukanov, A., Consiglio, L., D'Ambrosio, N., De Lellis, G., De Serio, M., ... Zghiche, A. (2014). Measurement of the TeV atmospheric muon charge ratio with the complete OPERA data set. European Physical Journal C, 74(7), 1-9. [2933]. https://doi.org/10.1140/epjc/s10052-014-2933-0

Agafonova, N, Aleksandrov, A, Anokhina, A, Aoki, S, Ariga, A, Ariga, T, Bender, D, Bertolin, A, Bozza, C, Brugnera, R, Buonaura, A, Buontempo, S, Büttner, B, Chernyavsky, M, Chukanov, A, Consiglio, L, D'Ambrosio, N, De Lellis, G, De Serio, M, Del Amo Sanchez, P, Di Crescenzo, A, Di Ferdinando, D, Di Marco, N, Dmitrievski, S, Dracos, M, Duchesneau, D, Dusini, S, Dzhatdoev, T, Ebert, J, Ereditato, A, Fini, RA, Fukuda, T, Galati, G, Garfagnini, A, Giacomelli, G, Göllnitz, C, Goldberg, J, Gornushkin, Y, Grella, G, Guler, M, Gustavino, C, Hagner, C, Hara, T, Hollnagel, A, Hosseini, B, Ishida, H, Ishiguro, K, Jakovcic, K, Jollet, C, Kamiscioglu, C, Kamiscioglu, M, Kawada, J, Kim, JH, Kim, SH, Kitagawa, N, Klicek, B, Kodama, K, Komatsu, M, Kose, U, Kreslo, I, Lauria, A, Lenkeit, J, Ljubicic, A, Longhin, A, Loverre, P, Malgin, A, Malenica, M, Mandrioli, G, Matsuo, T, Matveev, V, Mauri, N, Medinaceli, E, Meregaglia, A, Mikado, S, Monacelli, P, Montesi, MC, Morishima, K, Muciaccia, MT, Naganawa, N, Naka, T, Nakamura, M, Nakano, T, Nakatsuka, Y, Niwa, K, Ogawa, S, Okateva, N, Olshevsky, A, Omura, T, Ozaki, K, Paoloni, A, Park, BD, Park, IG, Pasqualini, L, Pastore, A, Patrizii, L, Pessard, H, Pistillo, C, Podgrudkov, D, Polukhina, N, Pozzato, M, Pupilli, F, Roda, M, Rokujo, H, Roganova, T, Rosa, G, Ryazhskaya, O, Sato, O, Schembri, A, Shakiryanova, I, Shchedrina, T, Sheshukov, A, Shibuya, H, Shiraishi, T, Shoziyoev, G, Simone, S, Sioli, M, Sirignano, C, Sirri, G, Spinetti, M, Stanco, L, Starkov, N, Stellacci, SM, Stipcevic, M, Strolin, P, Takahashi, S, Tenti, M, Terranova, F, Tioukov, V, Tufanli, S, Vilain, P, Vladimirov, M, Votano, L, Vuilleumier, JL, Wilquet, G, Wonsak, B, Yoon, CS, Zemskova, S & Zghiche, A 2014, 'Measurement of the TeV atmospheric muon charge ratio with the complete OPERA data set', European Physical Journal C, vol. 74, no. 7, 2933, pp. 1-9. https://doi.org/10.1140/epjc/s10052-014-2933-0

@article{8cdc1c7bad4f4a2cb3f3cf8ba8d3c38d,

title = "Measurement of the TeV atmospheric muon charge ratio with the complete OPERA data set",

abstract = "The OPERA detector, designed to search for νμ → ντ oscillations in the CNGS beam, is located in the underground Gran Sasso laboratory, a privileged location to study TeV-scale cosmic rays. For the analysis here presented, the detector was used to measure the atmospheric muon charge ratio in the TeV region. OPERA collected chargeseparated cosmic ray data between 2008 and 2012. More than 3 million atmospheric muon events were detected and reconstructed, among which about 110000 multiple muon bundles. The charge ratio Rμ ≡ Nμ+/Nμ − was measured separately for single and for multiple muon events. The analysis exploited the inversion of the magnet polarity which was performed on purpose during the 2012 Run. The combination of the two data sets with opposite magnet polarities allowedminimizing systematic uncertainties and reaching an accurate determination of the muon charge ratio. Data were fitted to obtain relevant parameters on the composition of primary cosmic rays and the associated kaon production in the forward fragmentation region. In the surface energy range 1–20 TeV investigated by OPERA, Rμ is well described by a parametric model including only pion and kaon contributions to themuon flux, showing no significant contribution of the prompt component. The energy independence supports the validity of Feynman scaling in the fragmentation region up to 200 TeV/nucleon primary energy.",

author = "N. Agafonova and A. Aleksandrov and A. Anokhina and S. Aoki and A. Ariga and T. Ariga and D. Bender and A. Bertolin and C. Bozza and R. Brugnera and A. Buonaura and S. Buontempo and B. B{\"u}ttner and M. Chernyavsky and A. Chukanov and L. Consiglio and N. D'Ambrosio and {De Lellis}, G. and {De Serio}, M. and {Del Amo Sanchez}, P. and {Di Crescenzo}, A. and {Di Ferdinando}, D. and {Di Marco}, N. and S. Dmitrievski and M. Dracos and D. Duchesneau and S. Dusini and T. Dzhatdoev and J. Ebert and A. Ereditato and Fini, {R. A.} and T. Fukuda and G. Galati and A. Garfagnini and G. Giacomelli and C. G{\"o}llnitz and J. Goldberg and Y. Gornushkin and G. Grella and M. Guler and C. Gustavino and C. Hagner and T. Hara and A. Hollnagel and B. Hosseini and H. Ishida and K. Ishiguro and K. Jakovcic and C. Jollet and C. Kamiscioglu and M. Kamiscioglu and J. Kawada and Kim, {J. H.} and Kim, {S. H.} and N. Kitagawa and B. Klicek and K. Kodama and M. Komatsu and U. Kose and I. Kreslo and A. Lauria and J. Lenkeit and A. Ljubicic and A. Longhin and P. Loverre and A. Malgin and M. Malenica and G. Mandrioli and T. Matsuo and V. Matveev and N. Mauri and E. Medinaceli and A. Meregaglia and S. Mikado and P. Monacelli and Montesi, {M. C.} and K. Morishima and Muciaccia, {M. T.} and N. Naganawa and T. Naka and M. Nakamura and T. Nakano and Y. Nakatsuka and K. Niwa and S. Ogawa and N. Okateva and A. Olshevsky and T. Omura and K. Ozaki and A. Paoloni and Park, {B. D.} and Park, {I. G.} and L. Pasqualini and A. Pastore and L. Patrizii and H. Pessard and C. Pistillo and D. Podgrudkov and N. Polukhina and M. Pozzato and F. Pupilli and M. Roda and H. Rokujo and T. Roganova and G. Rosa and O. Ryazhskaya and O. Sato and A. Schembri and I. Shakiryanova and T. Shchedrina and A. Sheshukov and H. Shibuya and T. Shiraishi and G. Shoziyoev and S. Simone and M. Sioli and C. Sirignano and G. Sirri and M. Spinetti and L. Stanco and N. Starkov and Stellacci, {S. M.} and M. Stipcevic and P. Strolin and S. Takahashi and M. Tenti and F. Terranova and V. Tioukov and S. Tufanli and P. Vilain and M. Vladimirov and L. Votano and Vuilleumier, {J. L.} and G. Wilquet and B. Wonsak and Yoon, {C. S.} and S. Zemskova and A. Zghiche",

note = "Funding Information: We thank CERN for the successful operation of the CNGS facility and INFN for the continuous support given to the experiment during the construction, installation and commissioning phases through its LNGS laboratory. We warmly acknowledge funding from our national agencies: Fonds de la Recherche Scientifique-FNRS and Institut InterUniversitaire des Sciences Nucl{\'e}aires for Belgium, MoSES for Croatia, CNRS and IN2P3 for France, BMBF for Germany, INFN for Italy, JSPS (Japan Society for the Promotion of Science), MEXT (Ministry of Education, Culture, Sports, Science and Technology), QFPU (Global COE programme of Nagoya University, Quest for Fundamental Principles in the Universe supported by JSPS and MEXT) and Promotion and Mutual Aid Corporation for Private Schools of Japan for Japan, SNF and the University of Bern for Switzerland, the Russian Foundation for Basic Research (Grant no. 09-02-00300 a, 12-02-12142 ofim), the Programs of the Presidium of the Russian Academy of Sciences Neutrino physics and Experimental and theoretical research-es of fundamental interactions connected with work on the accelerator of CERN, the Programs of Support of Leading Schools (Grant no. 3517.2010.2), and the Ministry of Education and Science of the Russian Federation for Russia, the National Research Foundation of Korea Grant No. 2011-0029457 for Korea and TUBITAK, the Scientific and Technological Research Council of Turkey, for Turkey. We are also indebted to INFN for providing fellowships and grants to non-Italian researchers. We thank the IN2P3 Computing Centre (CC-IN2P3) for providing computing resources for the analysis and hosting the central database for the OPERA experiment. We are indebted to our technical collaborators for the excellent quality of their work over many years of design, prototyping and construction of the detector and of its facilities. Publisher Copyright: {\textcopyright} The Author(s) 2014.",

year = "2014",

month = jul,

day = "15",

doi = "10.1140/epjc/s10052-014-2933-0",

language = "English",

volume = "74",

pages = "1--9",

journal = "European Physical Journal C",

issn = "1434-6044",

publisher = "Springer New York",

number = "7",

}

TY - JOUR

T1 - Measurement of the TeV atmospheric muon charge ratio with the complete OPERA data set

AU - Agafonova, N.

AU - Aleksandrov, A.

AU - Anokhina, A.

AU - Aoki, S.

AU - Ariga, A.

AU - Ariga, T.

AU - Bender, D.

AU - Bertolin, A.

AU - Bozza, C.

AU - Brugnera, R.

AU - Buonaura, A.

AU - Buontempo, S.

AU - Büttner, B.

AU - Chernyavsky, M.

AU - Chukanov, A.

AU - Consiglio, L.

AU - D'Ambrosio, N.

AU - De Lellis, G.

AU - De Serio, M.

AU - Del Amo Sanchez, P.

AU - Di Crescenzo, A.

AU - Di Ferdinando, D.

AU - Di Marco, N.

AU - Dmitrievski, S.

AU - Dracos, M.

AU - Duchesneau, D.

AU - Dusini, S.

AU - Dzhatdoev, T.

AU - Ebert, J.

AU - Ereditato, A.

AU - Fini, R. A.

AU - Fukuda, T.

AU - Galati, G.

AU - Garfagnini, A.

AU - Giacomelli, G.

AU - Göllnitz, C.

AU - Goldberg, J.

AU - Gornushkin, Y.

AU - Grella, G.

AU - Guler, M.

AU - Gustavino, C.

AU - Hagner, C.

AU - Hara, T.

AU - Hollnagel, A.

AU - Hosseini, B.

AU - Ishida, H.

AU - Ishiguro, K.

AU - Jakovcic, K.

AU - Jollet, C.

AU - Kamiscioglu, C.

AU - Kamiscioglu, M.

AU - Kawada, J.

AU - Kim, J. H.

AU - Kim, S. H.

AU - Kitagawa, N.

AU - Klicek, B.

AU - Kodama, K.

AU - Komatsu, M.

AU - Kose, U.

AU - Kreslo, I.

AU - Lauria, A.

AU - Lenkeit, J.

AU - Ljubicic, A.

AU - Longhin, A.

AU - Loverre, P.

AU - Malgin, A.

AU - Malenica, M.

AU - Mandrioli, G.

AU - Matsuo, T.

AU - Matveev, V.

AU - Mauri, N.

AU - Medinaceli, E.

AU - Meregaglia, A.

AU - Mikado, S.

AU - Monacelli, P.

AU - Montesi, M. C.

AU - Morishima, K.

AU - Muciaccia, M. T.

AU - Naganawa, N.

AU - Naka, T.

AU - Nakamura, M.

AU - Nakano, T.

AU - Nakatsuka, Y.

AU - Niwa, K.

AU - Ogawa, S.

AU - Okateva, N.

AU - Olshevsky, A.

AU - Omura, T.

AU - Ozaki, K.

AU - Paoloni, A.

AU - Park, B. D.

AU - Park, I. G.

AU - Pasqualini, L.

AU - Pastore, A.

AU - Patrizii, L.

AU - Pessard, H.

AU - Pistillo, C.

AU - Podgrudkov, D.

AU - Polukhina, N.

AU - Pozzato, M.

AU - Pupilli, F.

AU - Roda, M.

AU - Rokujo, H.

AU - Roganova, T.

AU - Rosa, G.

AU - Ryazhskaya, O.

AU - Sato, O.

AU - Schembri, A.

AU - Shakiryanova, I.

AU - Shchedrina, T.

AU - Sheshukov, A.

AU - Shibuya, H.

AU - Shiraishi, T.

AU - Shoziyoev, G.

AU - Simone, S.

AU - Sioli, M.

AU - Sirignano, C.

AU - Sirri, G.

AU - Spinetti, M.

AU - Stanco, L.

AU - Starkov, N.

AU - Stellacci, S. M.

AU - Stipcevic, M.

AU - Strolin, P.

AU - Takahashi, S.

AU - Tenti, M.

AU - Terranova, F.

AU - Tioukov, V.

AU - Tufanli, S.

AU - Vilain, P.

AU - Vladimirov, M.

AU - Votano, L.

AU - Vuilleumier, J. L.

AU - Wilquet, G.

AU - Wonsak, B.

AU - Yoon, C. S.

AU - Zemskova, S.

AU - Zghiche, A.

N1 - Funding Information: We thank CERN for the successful operation of the CNGS facility and INFN for the continuous support given to the experiment during the construction, installation and commissioning phases through its LNGS laboratory. We warmly acknowledge funding from our national agencies: Fonds de la Recherche Scientifique-FNRS and Institut InterUniversitaire des Sciences Nucléaires for Belgium, MoSES for Croatia, CNRS and IN2P3 for France, BMBF for Germany, INFN for Italy, JSPS (Japan Society for the Promotion of Science), MEXT (Ministry of Education, Culture, Sports, Science and Technology), QFPU (Global COE programme of Nagoya University, Quest for Fundamental Principles in the Universe supported by JSPS and MEXT) and Promotion and Mutual Aid Corporation for Private Schools of Japan for Japan, SNF and the University of Bern for Switzerland, the Russian Foundation for Basic Research (Grant no. 09-02-00300 a, 12-02-12142 ofim), the Programs of the Presidium of the Russian Academy of Sciences Neutrino physics and Experimental and theoretical research-es of fundamental interactions connected with work on the accelerator of CERN, the Programs of Support of Leading Schools (Grant no. 3517.2010.2), and the Ministry of Education and Science of the Russian Federation for Russia, the National Research Foundation of Korea Grant No. 2011-0029457 for Korea and TUBITAK, the Scientific and Technological Research Council of Turkey, for Turkey. We are also indebted to INFN for providing fellowships and grants to non-Italian researchers. We thank the IN2P3 Computing Centre (CC-IN2P3) for providing computing resources for the analysis and hosting the central database for the OPERA experiment. We are indebted to our technical collaborators for the excellent quality of their work over many years of design, prototyping and construction of the detector and of its facilities. Publisher Copyright: © The Author(s) 2014.

PY - 2014/7/15

Y1 - 2014/7/15

N2 - The OPERA detector, designed to search for νμ → ντ oscillations in the CNGS beam, is located in the underground Gran Sasso laboratory, a privileged location to study TeV-scale cosmic rays. For the analysis here presented, the detector was used to measure the atmospheric muon charge ratio in the TeV region. OPERA collected chargeseparated cosmic ray data between 2008 and 2012. More than 3 million atmospheric muon events were detected and reconstructed, among which about 110000 multiple muon bundles. The charge ratio Rμ ≡ Nμ+/Nμ − was measured separately for single and for multiple muon events. The analysis exploited the inversion of the magnet polarity which was performed on purpose during the 2012 Run. The combination of the two data sets with opposite magnet polarities allowedminimizing systematic uncertainties and reaching an accurate determination of the muon charge ratio. Data were fitted to obtain relevant parameters on the composition of primary cosmic rays and the associated kaon production in the forward fragmentation region. In the surface energy range 1–20 TeV investigated by OPERA, Rμ is well described by a parametric model including only pion and kaon contributions to themuon flux, showing no significant contribution of the prompt component. The energy independence supports the validity of Feynman scaling in the fragmentation region up to 200 TeV/nucleon primary energy.

AB - The OPERA detector, designed to search for νμ → ντ oscillations in the CNGS beam, is located in the underground Gran Sasso laboratory, a privileged location to study TeV-scale cosmic rays. For the analysis here presented, the detector was used to measure the atmospheric muon charge ratio in the TeV region. OPERA collected chargeseparated cosmic ray data between 2008 and 2012. More than 3 million atmospheric muon events were detected and reconstructed, among which about 110000 multiple muon bundles. The charge ratio Rμ ≡ Nμ+/Nμ − was measured separately for single and for multiple muon events. The analysis exploited the inversion of the magnet polarity which was performed on purpose during the 2012 Run. The combination of the two data sets with opposite magnet polarities allowedminimizing systematic uncertainties and reaching an accurate determination of the muon charge ratio. Data were fitted to obtain relevant parameters on the composition of primary cosmic rays and the associated kaon production in the forward fragmentation region. In the surface energy range 1–20 TeV investigated by OPERA, Rμ is well described by a parametric model including only pion and kaon contributions to themuon flux, showing no significant contribution of the prompt component. The energy independence supports the validity of Feynman scaling in the fragmentation region up to 200 TeV/nucleon primary energy.

UR - http://www.scopus.com/inward/record.url?scp=84903419850&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84903419850&partnerID=8YFLogxK

U2 - 10.1140/epjc/s10052-014-2933-0

DO - 10.1140/epjc/s10052-014-2933-0

M3 - Article

AN - SCOPUS:84903419850

SN - 1434-6044

VL - 74

SP - 1

EP - 9

JO - European Physical Journal C

JF - European Physical Journal C

IS - 7

M1 - 2933

ER -

Measurement of the TeV atmospheric muon charge ratio with the complete OPERA data set

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