Página principal > Measurement of TeV atmospheric muon charge ratio with the full OPERA data |
Article | |
Report number | arXiv:1403.0244 |
Title | Measurement of TeV atmospheric muon charge ratio with the full OPERA data |
Author(s) |
Agafonova, N. (Moscow, INR) ; Anokhina, A. (Moscow State U.) ; Aoki, S. (Kobe U.) ; Ariga, A. (Bern U.) ; Ariga, T. (Bern U.) ; Bender, D. (Middle East Tech. U., Ankara) ; Bertolin, A. (INFN, Padua) ; Bozza, C. (Salerno U. ; INFN, Salerno) ; Brugnera, R. (Padua U. ; INFN, Padua) ; Buonaura, A. (Naples U. ; INFN, Naples) ; Buontempo, S. (INFN, Naples) ; Buttner, B. (Hamburg U., Inst. Theor. Phys. II) ; Chernyavsky, M. (Lebedev Inst.) ; Chukanov, A. (Dubna, JINR) ; Consiglio, L. (INFN, Naples) ; D'Ambrosio, N. (Gran Sasso) ; De Lellis, G. (Naples U. ; INFN, Naples) ; De Serio, M. (Bari U. ; INFN, Bari) ; del Amo Sanchez, P. (Annecy, LAPP) ; Di Crescenzo, A. (INFN, Naples) ; Di Ferdinando, D. (INFN, Bologna) ; Di Marco, N. (Gran Sasso) ; Dmitrievski, S. (Dubna, JINR) ; Dracos, M. (Louis Pasteur U., Strasbourg I) ; Duchesneau, D. (Annecy, LAPP) ; Dusini, S. (INFN, Padua) ; Dzhatdoev, T. (Moscow State U.) ; Ebert, J. (Hamburg U., Inst. Theor. Phys. II) ; Ereditato, A. (Bern U.) ; Fini, R.A. (INFN, Bari) ; Fukuda, T. (Toho U.) ; Galati, G. (Bari U. ; INFN, Bari) ; Garfagnini, A. (Padua U. ; INFN, Padua) ; Giacomelli, G. (Bologna U. ; INFN, Bologna) ; Gollnitz, C. (Hamburg U., Inst. Theor. Phys. II) ; Goldberg, J. (Technion) ; Gornushkin, Y. (Dubna, JINR) ; Grella, G. (Salerno U. ; INFN, Salerno) ; Guler, M. (Middle East Tech. U., Ankara) ; Gustavino, C. (INFN, Rome) ; Hagner, C. (Hamburg U., Inst. Theor. Phys. II) ; Hara, T. (Kobe U.) ; Hollnagel, A. (Hamburg U., Inst. Theor. Phys. II) ; Hosseini, B. (Naples U. ; INFN, Naples) ; Ishida, H. (Toho U.) ; Ishiguro, K. (Nagoya U.) ; Jakovcic, K. (Boskovic Inst., Zagreb) ; Jollet, C. (Louis Pasteur U., Strasbourg I) ; Kamiscioglu, C. (Middle East Tech. U., Ankara) ; Kamiscioglu, M. (Middle East Tech. U., Ankara) ; Kawada, J. (Bern U.) ; Kim, J.H. (Gyeongsang Natl. U.) ; Kim, S.H. (Gyeongsang Natl. U.) ; Kitagawa, N. (Nagoya U.) ; Klicek, B. (Boskovic Inst., Zagreb) ; Kodama, K. (Aichi U.) ; Komatsu, M. (Nagoya U.) ; Kose, U. (INFN, Padua) ; Kreslo, I. (Bern U.) ; Lauria, A. (Naples U. ; INFN, Naples) ; Lenkeit, J. (Hamburg U., Inst. Theor. Phys. II) ; Ljubicic, A. (Boskovic Inst., Zagreb) ; Longhin, A. (INFN, Rome) ; Loverre, P. (Rome U. ; INFN, Rome) ; Malgin, A. (Moscow, INR) ; Malenica, M. (Boskovic Inst., Zagreb) ; Mandrioli, G. (INFN, Bologna) ; Matsuo, T. (Toho U.) ; Matveev, V. (Moscow, INR) ; Mauri, N. (Bologna U. ; INFN, Bologna) ; Medinaceli, E. (Padua U. ; INFN, Padua) ; Meregaglia, A. (Louis Pasteur U., Strasbourg I) ; Mikado, S. (Nihon U., Narashino) ; Monacelli, P. (INFN, Rome) ; Montesi, M.C. (Naples U. ; INFN, Naples) ; Morishima, K. (Nagoya U.) ; Muciaccia, M.T. (Bari U. ; INFN, Bari) ; Naganawa, N. (Nagoya U.) ; Naka, T. (Nagoya U.) ; Nakamura, M. (Nagoya U.) ; Nakano, T. (Nagoya U.) ; Nakatsuka, Y. (Nagoya U.) ; Niwa, K. (Nagoya U.) ; Ogawa, S. (Toho U.) ; Okateva, N. (Lebedev Inst.) ; Olshevsky, A. (Dubna, JINR) ; Omura, T. (Nagoya U.) ; Ozaki, K. (Kobe U.) ; Paoloni, A. (INFN, Rome) ; Park, B.D. (Gyeongsang Natl. U.) ; Park, I.G. (Gyeongsang Natl. U.) ; Pasqualini, L. (Bologna U. ; INFN, Bologna) ; Pastore, A. (INFN, Bari) ; Patrizii, L. (INFN, Bologna) ; Pessard, H. (Annecy, LAPP) ; Pistillo, C. (Bern U.) ; Podgrudkov, D. (Moscow State U.) ; Polukhina, N. (Lebedev Inst.) ; Pozzato, M. (Bologna U. ; INFN, Bologna) ; Pupilli, F. (Gran Sasso) ; Roda, M. (Padua U. ; INFN, Padua) ; Rokujo, H. (Nagoya U.) ; Roganova, T. (Moscow State U.) ; Rosa, G. (Rome U. ; INFN, Rome) ; Ryazhskaya, O. (Moscow, INR) ; Sato, O. (Nagoya U.) ; Schembri, A. (Gran Sasso) ; Shakiryanova, I. (Moscow, INR) ; Shchedrina, T. (INFN, Naples) ; Sheshukov, A. (Dubna, JINR) ; Shibuya, H. (Toho U.) ; Shiraishi, T. (Nagoya U.) ; Shoziyoev, G. (Moscow State U.) ; Simone, S. (Bari U. ; INFN, Bari) ; Sioli, M. (Bologna U. ; INFN, Bologna) ; Sirignano, C. (Padua U. ; INFN, Padua) ; Sirri, G. (INFN, Bologna) ; Spinetti, M. (INFN, Rome) ; Stanco, L. (INFN, Padua) ; Starkov, N. (Lebedev Inst.) ; Stellacci, S.M. (Salerno U. ; INFN, Salerno) ; Stipcevic, M. (Boskovic Inst., Zagreb) ; Strolin, P. (Naples U. ; INFN, Naples) ; Takahashi, S. (Kobe U.) ; Tenti, M. (Bologna U. ; INFN, Bologna) ; Terranova, F. (INFN, Rome ; Milan U.) ; Tioukov, V. (INFN, Naples) ; Tufanli, S. (Bern U.) ; Vilain, P. (Brussels U.) ; Vladimirov, M. (Lebedev Inst.) ; Votano, L. (INFN, Rome) ; Vuilleumier, J.L. (Bern U.) ; Wilquet, G. (Brussels U.) ; Wonsak, B. (Hamburg U., Inst. Theor. Phys. II) ; Yoon, C.S. (Gyeongsang Natl. U.) ; Zemskova, S. (Dubna, JINR) ; Zghiche, A. (Annecy, LAPP) |
Publication | 2014-07-02 |
Imprint | 02 Mar 2014 |
Number of pages | 9 |
Note | Comments: 8 pages, 2 figures, 4 tables 8 pages, 2 figures, 4 tables |
In: | Eur. Phys. J. C 74 (2014) pp.2933 |
DOI | 10.1140/epjc/s10052-014-2933-0 10.1140/epjc/s10052-014-2933-0 |
Subject category | Particle Physics - Experiment |
Accelerator/Facility, Experiment | CERN SPS ; OPERA CNGS1 |
Abstract | The OPERA detector, designed to search for ν μ → ν τ 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 charge- separated 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 anal- ysis exploited the inversion of the magnet polarity which was performed on purpose during the 2012 Run. The com- bination of the two data sets with opposite magnet polarities allowedminimizingsystematicuncertaintiesandreachingan accurate determination of the muon charge ratio. Data were fittedtoobtainrelevant parametersonthecompositionofpri- mary 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 contribu- tions to the muon 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 |
Copyright/License | arXiv nonexclusive-distrib. 1.0 |