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.
| 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 | |
| Publication status | Published - Jul 15 2014 |
| Externally published | Yes |
All Science Journal Classification (ASJC) codes
- Engineering (miscellaneous)
- Physics and Astronomy (miscellaneous)
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Measurement of the TeV atmospheric muon charge ratio with the complete OPERA data set. / 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, R. A.; 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, J. H.; Kim, S. H.; 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, M. C.; Morishima, K.; Muciaccia, M. T.; 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, B. D.; Park, I. G.; 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, S. M.; Stipcevic, M.; Strolin, P.; Takahashi, S.; Tenti, M.; Terranova, F.; Tioukov, V.; Tufanli, S.; Vilain, P.; Vladimirov, M.; Votano, L.; Vuilleumier, J. L.; Wilquet, G.; Wonsak, B.; Yoon, C. S.; Zemskova, S.; Zghiche, A.
In: European Physical Journal C, Vol. 74, No. 7, 2933, 15.07.2014, p. 1-9.Research output: Contribution to journal › Article › peer-review
}
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
VL - 74
SP - 1
EP - 9
JO - European Physical Journal C
JF - European Physical Journal C
SN - 1434-6044
IS - 7
M1 - 2933
ER -