Final results of the search for νμ → νe oscillations with the OPERA detector in the CNGS beam
Abstract The OPERA experiment has discovered the tau neutrino appearance in the CNGS muon neutrino beam, in agreement with the 3 neutrino flavour oscillation hypothesis. The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electr...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Agafonova, N. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2018 |
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| Schlagwörter: |
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| Anmerkung: |
© The Author(s) 2018 |
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| Übergeordnetes Werk: |
Enthalten in: Journal of high energy physics - Berlin : Springer, 1997, 2018(2018), 6 vom: 27. Juni |
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| Übergeordnetes Werk: |
volume:2018 ; year:2018 ; number:6 ; day:27 ; month:06 |
| Links: |
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| DOI / URN: |
10.1007/JHEP06(2018)151 |
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| Katalog-ID: |
SPR030560802 |
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| 100 | 1 | |a Agafonova, N. |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Final results of the search for νμ → νe oscillations with the OPERA detector in the CNGS beam |
| 264 | 1 | |c 2018 | |
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| 520 | |a Abstract The OPERA experiment has discovered the tau neutrino appearance in the CNGS muon neutrino beam, in agreement with the 3 neutrino flavour oscillation hypothesis. The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electromagnetic showers. Moreover, thanks to the very high granularity of the emulsion films, showers induced by electrons can be distinguished from those induced by π0s, thus allowing the detection of charged current interactions of electron neutrinos. In this paper the results of the search for electron neutrino events using the full dataset are reported. An improved method for the electron neutrino energy estimation is exploited. Data are compatible with the 3 neutrino flavour mixing model expectations and are used to set limits on the oscillation parameters of the 3+1 neutrino mixing model, in which an additional mass eigenstate m4 is introduced. At high Δm412 (≳0.1 $ eV^{2} $), an upper limit on $ sin^{2} $ 2θμe is set to 0.021 at 90% C.L. and Δm412 ≳ 4 × $ 10^{− 3} $ $ eV^{2} $ is excluded for maximal mixing in appearance mode. | ||
| 650 | 4 | |a Neutrino Detectors and Telescopes (experiments) |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Oscillation |7 (dpeaa)DE-He213 | |
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| 700 | 1 | |a Buontempo, S. |4 aut | |
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| 700 | 1 | |a Consiglio, L. |4 aut | |
| 700 | 1 | |a D’Ambrosio, N. |4 aut | |
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| 700 | 1 | |a Di Marco, N. |4 aut | |
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10.1007/JHEP06(2018)151 doi (DE-627)SPR030560802 (SPR)JHEP06(2018)151-e DE-627 ger DE-627 rakwb eng Agafonova, N. verfasserin aut Final results of the search for νμ → νe oscillations with the OPERA detector in the CNGS beam 2018 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s) 2018 Abstract The OPERA experiment has discovered the tau neutrino appearance in the CNGS muon neutrino beam, in agreement with the 3 neutrino flavour oscillation hypothesis. The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electromagnetic showers. Moreover, thanks to the very high granularity of the emulsion films, showers induced by electrons can be distinguished from those induced by π0s, thus allowing the detection of charged current interactions of electron neutrinos. In this paper the results of the search for electron neutrino events using the full dataset are reported. An improved method for the electron neutrino energy estimation is exploited. Data are compatible with the 3 neutrino flavour mixing model expectations and are used to set limits on the oscillation parameters of the 3+1 neutrino mixing model, in which an additional mass eigenstate m4 is introduced. At high Δm412 (≳0.1 $ eV^{2} $), an upper limit on $ sin^{2} $ 2θμe is set to 0.021 at 90% C.L. and Δm412 ≳ 4 × $ 10^{− 3} $ $ eV^{2} $ is excluded for maximal mixing in appearance mode. Neutrino Detectors and Telescopes (experiments) (dpeaa)DE-He213 Oscillation (dpeaa)DE-He213 Aleksandrov, A. aut Anokhina, A. aut Aoki, S. aut Ariga, A. aut Ariga, T. aut Bertolin, A. aut Bozza, C. aut Brugnera, R. aut Buonaura, A. aut Buontempo, S. aut Chernyavskiy, M. aut Chukanov, A. aut Consiglio, L. aut D’Ambrosio, N. aut De Lellis, G. aut De Serio, M. aut del Amo Sanchez, P. aut Di Crescenzo, A. aut Di Ferdinando, D. aut Di Marco, N. aut Dmitrievsky, S. aut Dracos, M. aut Duchesneau, D. aut Dusini, S. aut Dzhatdoev, T. aut Ebert, J. aut Ereditato, A. aut Favier, J. aut Fini, R. A. aut Fornari, F. aut Fukuda, T. aut Galati, G. aut Garfagnini, A. aut Gentile, V. aut Goldberg, J. aut Gornushkin, Y. aut Gorbunov, S. aut Grella, G. aut Guler, A. M. aut Gustavino, C. aut Hagner, C. aut Hara, T. aut Hayakawa, T. aut Hollnagel, A. aut Hosseini, B. aut Ishiguro, K. aut Iuliano, A. aut Jakovcic, K. aut Jollet, C. aut Kamiscioglu, C. aut Kamiscioglu, M. aut Kim, S. H. aut Kitagawa, N. aut Klicek, B. aut Kodama, K. aut Komatsu, M. aut Kose, U. aut Kreslo, I. aut Laudisio, F. aut Lauria, A. aut Ljubicic, A. aut Longhin, A. aut Loverre, P. aut Malgin, A. aut Malenica, M. aut Mandrioli, G. aut Matsuo, T. aut Matveev, V. aut Mauri, N. aut Medinaceli, E. aut Meisel, F. aut Meregaglia, A. aut Mikado, S. aut Miyanishi, M. aut Mizutani, F. aut Monacelli, P. aut Montesi, M. C. aut Morishima, K. aut Muciaccia, M. T. aut Naganawa, N. aut Naka, T. aut Nakamura, M. aut Nakano, T. aut Niwa, K. aut Okateva, N. aut Ogawa, S. aut Ozaki, K. aut Paoloni, A. aut Paparella, L. aut Park, B. D. aut Pasqualini, L. aut Pastore, A. aut Patrizii, L. aut Pessard, H. aut Podgrudkov, D. aut Polukhina, N. aut Pozzato, M. aut Pupilli, F. aut Roda, M. aut Roganova, T. aut Rokujo, H. aut Rosa, G. aut Ryazhskaya, O. aut Sato, O. aut Schembri, A. aut Shakiryanova, I. aut Shchedrina, T. aut Shibuya, H. aut Shibayama, E. aut Shiraishi, T. aut Simone, S. aut Sirignano, C. aut Sirri, G. aut Sotnikov, A. aut Spinetti, M. aut Stanco, L. aut Starkov, N. aut Stellacci, S. M. aut Stipcevic, M. aut Strolin, P. aut Takahashi, S. aut Tenti, M. aut Terranova, F. aut Tioukov, V. aut Vasina, S. aut Vilain, P. aut Voevodina, E. aut Votano, L. aut Vuilleumier, J. L. aut Wilquet, G. aut Yoon, C. S. aut Enthalten in Journal of high energy physics Berlin : Springer, 1997 2018(2018), 6 vom: 27. Juni (DE-627)320910571 (DE-600)2027350-2 1029-8479 nnns volume:2018 year:2018 number:6 day:27 month:06 https://dx.doi.org/10.1007/JHEP06(2018)151 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2014 GBV_ILN_2020 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 2018 2018 6 27 06 |
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10.1007/JHEP06(2018)151 doi (DE-627)SPR030560802 (SPR)JHEP06(2018)151-e DE-627 ger DE-627 rakwb eng Agafonova, N. verfasserin aut Final results of the search for νμ → νe oscillations with the OPERA detector in the CNGS beam 2018 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s) 2018 Abstract The OPERA experiment has discovered the tau neutrino appearance in the CNGS muon neutrino beam, in agreement with the 3 neutrino flavour oscillation hypothesis. The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electromagnetic showers. Moreover, thanks to the very high granularity of the emulsion films, showers induced by electrons can be distinguished from those induced by π0s, thus allowing the detection of charged current interactions of electron neutrinos. In this paper the results of the search for electron neutrino events using the full dataset are reported. An improved method for the electron neutrino energy estimation is exploited. Data are compatible with the 3 neutrino flavour mixing model expectations and are used to set limits on the oscillation parameters of the 3+1 neutrino mixing model, in which an additional mass eigenstate m4 is introduced. At high Δm412 (≳0.1 $ eV^{2} $), an upper limit on $ sin^{2} $ 2θμe is set to 0.021 at 90% C.L. and Δm412 ≳ 4 × $ 10^{− 3} $ $ eV^{2} $ is excluded for maximal mixing in appearance mode. Neutrino Detectors and Telescopes (experiments) (dpeaa)DE-He213 Oscillation (dpeaa)DE-He213 Aleksandrov, A. aut Anokhina, A. aut Aoki, S. aut Ariga, A. aut Ariga, T. aut Bertolin, A. aut Bozza, C. aut Brugnera, R. aut Buonaura, A. aut Buontempo, S. aut Chernyavskiy, M. aut Chukanov, A. aut Consiglio, L. aut D’Ambrosio, N. aut De Lellis, G. aut De Serio, M. aut del Amo Sanchez, P. aut Di Crescenzo, A. aut Di Ferdinando, D. aut Di Marco, N. aut Dmitrievsky, S. aut Dracos, M. aut Duchesneau, D. aut Dusini, S. aut Dzhatdoev, T. aut Ebert, J. aut Ereditato, A. aut Favier, J. aut Fini, R. A. aut Fornari, F. aut Fukuda, T. aut Galati, G. aut Garfagnini, A. aut Gentile, V. aut Goldberg, J. aut Gornushkin, Y. aut Gorbunov, S. aut Grella, G. aut Guler, A. M. aut Gustavino, C. aut Hagner, C. aut Hara, T. aut Hayakawa, T. aut Hollnagel, A. aut Hosseini, B. aut Ishiguro, K. aut Iuliano, A. aut Jakovcic, K. aut Jollet, C. aut Kamiscioglu, C. aut Kamiscioglu, M. aut Kim, S. H. aut Kitagawa, N. aut Klicek, B. aut Kodama, K. aut Komatsu, M. aut Kose, U. aut Kreslo, I. aut Laudisio, F. aut Lauria, A. aut Ljubicic, A. aut Longhin, A. aut Loverre, P. aut Malgin, A. aut Malenica, M. aut Mandrioli, G. aut Matsuo, T. aut Matveev, V. aut Mauri, N. aut Medinaceli, E. aut Meisel, F. aut Meregaglia, A. aut Mikado, S. aut Miyanishi, M. aut Mizutani, F. aut Monacelli, P. aut Montesi, M. C. aut Morishima, K. aut Muciaccia, M. T. aut Naganawa, N. aut Naka, T. aut Nakamura, M. aut Nakano, T. aut Niwa, K. aut Okateva, N. aut Ogawa, S. aut Ozaki, K. aut Paoloni, A. aut Paparella, L. aut Park, B. D. aut Pasqualini, L. aut Pastore, A. aut Patrizii, L. aut Pessard, H. aut Podgrudkov, D. aut Polukhina, N. aut Pozzato, M. aut Pupilli, F. aut Roda, M. aut Roganova, T. aut Rokujo, H. aut Rosa, G. aut Ryazhskaya, O. aut Sato, O. aut Schembri, A. aut Shakiryanova, I. aut Shchedrina, T. aut Shibuya, H. aut Shibayama, E. aut Shiraishi, T. aut Simone, S. aut Sirignano, C. aut Sirri, G. aut Sotnikov, A. aut Spinetti, M. aut Stanco, L. aut Starkov, N. aut Stellacci, S. M. aut Stipcevic, M. aut Strolin, P. aut Takahashi, S. aut Tenti, M. aut Terranova, F. aut Tioukov, V. aut Vasina, S. aut Vilain, P. aut Voevodina, E. aut Votano, L. aut Vuilleumier, J. L. aut Wilquet, G. aut Yoon, C. S. aut Enthalten in Journal of high energy physics Berlin : Springer, 1997 2018(2018), 6 vom: 27. Juni (DE-627)320910571 (DE-600)2027350-2 1029-8479 nnns volume:2018 year:2018 number:6 day:27 month:06 https://dx.doi.org/10.1007/JHEP06(2018)151 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2014 GBV_ILN_2020 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 2018 2018 6 27 06 |
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10.1007/JHEP06(2018)151 doi (DE-627)SPR030560802 (SPR)JHEP06(2018)151-e DE-627 ger DE-627 rakwb eng Agafonova, N. verfasserin aut Final results of the search for νμ → νe oscillations with the OPERA detector in the CNGS beam 2018 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s) 2018 Abstract The OPERA experiment has discovered the tau neutrino appearance in the CNGS muon neutrino beam, in agreement with the 3 neutrino flavour oscillation hypothesis. The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electromagnetic showers. Moreover, thanks to the very high granularity of the emulsion films, showers induced by electrons can be distinguished from those induced by π0s, thus allowing the detection of charged current interactions of electron neutrinos. In this paper the results of the search for electron neutrino events using the full dataset are reported. An improved method for the electron neutrino energy estimation is exploited. Data are compatible with the 3 neutrino flavour mixing model expectations and are used to set limits on the oscillation parameters of the 3+1 neutrino mixing model, in which an additional mass eigenstate m4 is introduced. At high Δm412 (≳0.1 $ eV^{2} $), an upper limit on $ sin^{2} $ 2θμe is set to 0.021 at 90% C.L. and Δm412 ≳ 4 × $ 10^{− 3} $ $ eV^{2} $ is excluded for maximal mixing in appearance mode. Neutrino Detectors and Telescopes (experiments) (dpeaa)DE-He213 Oscillation (dpeaa)DE-He213 Aleksandrov, A. aut Anokhina, A. aut Aoki, S. aut Ariga, A. aut Ariga, T. aut Bertolin, A. aut Bozza, C. aut Brugnera, R. aut Buonaura, A. aut Buontempo, S. aut Chernyavskiy, M. aut Chukanov, A. aut Consiglio, L. aut D’Ambrosio, N. aut De Lellis, G. aut De Serio, M. aut del Amo Sanchez, P. aut Di Crescenzo, A. aut Di Ferdinando, D. aut Di Marco, N. aut Dmitrievsky, S. aut Dracos, M. aut Duchesneau, D. aut Dusini, S. aut Dzhatdoev, T. aut Ebert, J. aut Ereditato, A. aut Favier, J. aut Fini, R. A. aut Fornari, F. aut Fukuda, T. aut Galati, G. aut Garfagnini, A. aut Gentile, V. aut Goldberg, J. aut Gornushkin, Y. aut Gorbunov, S. aut Grella, G. aut Guler, A. M. aut Gustavino, C. aut Hagner, C. aut Hara, T. aut Hayakawa, T. aut Hollnagel, A. aut Hosseini, B. aut Ishiguro, K. aut Iuliano, A. aut Jakovcic, K. aut Jollet, C. aut Kamiscioglu, C. aut Kamiscioglu, M. aut Kim, S. H. aut Kitagawa, N. aut Klicek, B. aut Kodama, K. aut Komatsu, M. aut Kose, U. aut Kreslo, I. aut Laudisio, F. aut Lauria, A. aut Ljubicic, A. aut Longhin, A. aut Loverre, P. aut Malgin, A. aut Malenica, M. aut Mandrioli, G. aut Matsuo, T. aut Matveev, V. aut Mauri, N. aut Medinaceli, E. aut Meisel, F. aut Meregaglia, A. aut Mikado, S. aut Miyanishi, M. aut Mizutani, F. aut Monacelli, P. aut Montesi, M. C. aut Morishima, K. aut Muciaccia, M. T. aut Naganawa, N. aut Naka, T. aut Nakamura, M. aut Nakano, T. aut Niwa, K. aut Okateva, N. aut Ogawa, S. aut Ozaki, K. aut Paoloni, A. aut Paparella, L. aut Park, B. D. aut Pasqualini, L. aut Pastore, A. aut Patrizii, L. aut Pessard, H. aut Podgrudkov, D. aut Polukhina, N. aut Pozzato, M. aut Pupilli, F. aut Roda, M. aut Roganova, T. aut Rokujo, H. aut Rosa, G. aut Ryazhskaya, O. aut Sato, O. aut Schembri, A. aut Shakiryanova, I. aut Shchedrina, T. aut Shibuya, H. aut Shibayama, E. aut Shiraishi, T. aut Simone, S. aut Sirignano, C. aut Sirri, G. aut Sotnikov, A. aut Spinetti, M. aut Stanco, L. aut Starkov, N. aut Stellacci, S. M. aut Stipcevic, M. aut Strolin, P. aut Takahashi, S. aut Tenti, M. aut Terranova, F. aut Tioukov, V. aut Vasina, S. aut Vilain, P. aut Voevodina, E. aut Votano, L. aut Vuilleumier, J. L. aut Wilquet, G. aut Yoon, C. S. aut Enthalten in Journal of high energy physics Berlin : Springer, 1997 2018(2018), 6 vom: 27. Juni (DE-627)320910571 (DE-600)2027350-2 1029-8479 nnns volume:2018 year:2018 number:6 day:27 month:06 https://dx.doi.org/10.1007/JHEP06(2018)151 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2014 GBV_ILN_2020 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 2018 2018 6 27 06 |
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10.1007/JHEP06(2018)151 doi (DE-627)SPR030560802 (SPR)JHEP06(2018)151-e DE-627 ger DE-627 rakwb eng Agafonova, N. verfasserin aut Final results of the search for νμ → νe oscillations with the OPERA detector in the CNGS beam 2018 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s) 2018 Abstract The OPERA experiment has discovered the tau neutrino appearance in the CNGS muon neutrino beam, in agreement with the 3 neutrino flavour oscillation hypothesis. The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electromagnetic showers. Moreover, thanks to the very high granularity of the emulsion films, showers induced by electrons can be distinguished from those induced by π0s, thus allowing the detection of charged current interactions of electron neutrinos. In this paper the results of the search for electron neutrino events using the full dataset are reported. An improved method for the electron neutrino energy estimation is exploited. Data are compatible with the 3 neutrino flavour mixing model expectations and are used to set limits on the oscillation parameters of the 3+1 neutrino mixing model, in which an additional mass eigenstate m4 is introduced. At high Δm412 (≳0.1 $ eV^{2} $), an upper limit on $ sin^{2} $ 2θμe is set to 0.021 at 90% C.L. and Δm412 ≳ 4 × $ 10^{− 3} $ $ eV^{2} $ is excluded for maximal mixing in appearance mode. Neutrino Detectors and Telescopes (experiments) (dpeaa)DE-He213 Oscillation (dpeaa)DE-He213 Aleksandrov, A. aut Anokhina, A. aut Aoki, S. aut Ariga, A. aut Ariga, T. aut Bertolin, A. aut Bozza, C. aut Brugnera, R. aut Buonaura, A. aut Buontempo, S. aut Chernyavskiy, M. aut Chukanov, A. aut Consiglio, L. aut D’Ambrosio, N. aut De Lellis, G. aut De Serio, M. aut del Amo Sanchez, P. aut Di Crescenzo, A. aut Di Ferdinando, D. aut Di Marco, N. aut Dmitrievsky, S. aut Dracos, M. aut Duchesneau, D. aut Dusini, S. aut Dzhatdoev, T. aut Ebert, J. aut Ereditato, A. aut Favier, J. aut Fini, R. A. aut Fornari, F. aut Fukuda, T. aut Galati, G. aut Garfagnini, A. aut Gentile, V. aut Goldberg, J. aut Gornushkin, Y. aut Gorbunov, S. aut Grella, G. aut Guler, A. M. aut Gustavino, C. aut Hagner, C. aut Hara, T. aut Hayakawa, T. aut Hollnagel, A. aut Hosseini, B. aut Ishiguro, K. aut Iuliano, A. aut Jakovcic, K. aut Jollet, C. aut Kamiscioglu, C. aut Kamiscioglu, M. aut Kim, S. H. aut Kitagawa, N. aut Klicek, B. aut Kodama, K. aut Komatsu, M. aut Kose, U. aut Kreslo, I. aut Laudisio, F. aut Lauria, A. aut Ljubicic, A. aut Longhin, A. aut Loverre, P. aut Malgin, A. aut Malenica, M. aut Mandrioli, G. aut Matsuo, T. aut Matveev, V. aut Mauri, N. aut Medinaceli, E. aut Meisel, F. aut Meregaglia, A. aut Mikado, S. aut Miyanishi, M. aut Mizutani, F. aut Monacelli, P. aut Montesi, M. C. aut Morishima, K. aut Muciaccia, M. T. aut Naganawa, N. aut Naka, T. aut Nakamura, M. aut Nakano, T. aut Niwa, K. aut Okateva, N. aut Ogawa, S. aut Ozaki, K. aut Paoloni, A. aut Paparella, L. aut Park, B. D. aut Pasqualini, L. aut Pastore, A. aut Patrizii, L. aut Pessard, H. aut Podgrudkov, D. aut Polukhina, N. aut Pozzato, M. aut Pupilli, F. aut Roda, M. aut Roganova, T. aut Rokujo, H. aut Rosa, G. aut Ryazhskaya, O. aut Sato, O. aut Schembri, A. aut Shakiryanova, I. aut Shchedrina, T. aut Shibuya, H. aut Shibayama, E. aut Shiraishi, T. aut Simone, S. aut Sirignano, C. aut Sirri, G. aut Sotnikov, A. aut Spinetti, M. aut Stanco, L. aut Starkov, N. aut Stellacci, S. M. aut Stipcevic, M. aut Strolin, P. aut Takahashi, S. aut Tenti, M. aut Terranova, F. aut Tioukov, V. aut Vasina, S. aut Vilain, P. aut Voevodina, E. aut Votano, L. aut Vuilleumier, J. L. aut Wilquet, G. aut Yoon, C. S. aut Enthalten in Journal of high energy physics Berlin : Springer, 1997 2018(2018), 6 vom: 27. Juni (DE-627)320910571 (DE-600)2027350-2 1029-8479 nnns volume:2018 year:2018 number:6 day:27 month:06 https://dx.doi.org/10.1007/JHEP06(2018)151 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2014 GBV_ILN_2020 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 2018 2018 6 27 06 |
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10.1007/JHEP06(2018)151 doi (DE-627)SPR030560802 (SPR)JHEP06(2018)151-e DE-627 ger DE-627 rakwb eng Agafonova, N. verfasserin aut Final results of the search for νμ → νe oscillations with the OPERA detector in the CNGS beam 2018 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s) 2018 Abstract The OPERA experiment has discovered the tau neutrino appearance in the CNGS muon neutrino beam, in agreement with the 3 neutrino flavour oscillation hypothesis. The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electromagnetic showers. Moreover, thanks to the very high granularity of the emulsion films, showers induced by electrons can be distinguished from those induced by π0s, thus allowing the detection of charged current interactions of electron neutrinos. In this paper the results of the search for electron neutrino events using the full dataset are reported. An improved method for the electron neutrino energy estimation is exploited. Data are compatible with the 3 neutrino flavour mixing model expectations and are used to set limits on the oscillation parameters of the 3+1 neutrino mixing model, in which an additional mass eigenstate m4 is introduced. At high Δm412 (≳0.1 $ eV^{2} $), an upper limit on $ sin^{2} $ 2θμe is set to 0.021 at 90% C.L. and Δm412 ≳ 4 × $ 10^{− 3} $ $ eV^{2} $ is excluded for maximal mixing in appearance mode. Neutrino Detectors and Telescopes (experiments) (dpeaa)DE-He213 Oscillation (dpeaa)DE-He213 Aleksandrov, A. aut Anokhina, A. aut Aoki, S. aut Ariga, A. aut Ariga, T. aut Bertolin, A. aut Bozza, C. aut Brugnera, R. aut Buonaura, A. aut Buontempo, S. aut Chernyavskiy, M. aut Chukanov, A. aut Consiglio, L. aut D’Ambrosio, N. aut De Lellis, G. aut De Serio, M. aut del Amo Sanchez, P. aut Di Crescenzo, A. aut Di Ferdinando, D. aut Di Marco, N. aut Dmitrievsky, S. aut Dracos, M. aut Duchesneau, D. aut Dusini, S. aut Dzhatdoev, T. aut Ebert, J. aut Ereditato, A. aut Favier, J. aut Fini, R. A. aut Fornari, F. aut Fukuda, T. aut Galati, G. aut Garfagnini, A. aut Gentile, V. aut Goldberg, J. aut Gornushkin, Y. aut Gorbunov, S. aut Grella, G. aut Guler, A. M. aut Gustavino, C. aut Hagner, C. aut Hara, T. aut Hayakawa, T. aut Hollnagel, A. aut Hosseini, B. aut Ishiguro, K. aut Iuliano, A. aut Jakovcic, K. aut Jollet, C. aut Kamiscioglu, C. aut Kamiscioglu, M. aut Kim, S. H. aut Kitagawa, N. aut Klicek, B. aut Kodama, K. aut Komatsu, M. aut Kose, U. aut Kreslo, I. aut Laudisio, F. aut Lauria, A. aut Ljubicic, A. aut Longhin, A. aut Loverre, P. aut Malgin, A. aut Malenica, M. aut Mandrioli, G. aut Matsuo, T. aut Matveev, V. aut Mauri, N. aut Medinaceli, E. aut Meisel, F. aut Meregaglia, A. aut Mikado, S. aut Miyanishi, M. aut Mizutani, F. aut Monacelli, P. aut Montesi, M. C. aut Morishima, K. aut Muciaccia, M. T. aut Naganawa, N. aut Naka, T. aut Nakamura, M. aut Nakano, T. aut Niwa, K. aut Okateva, N. aut Ogawa, S. aut Ozaki, K. aut Paoloni, A. aut Paparella, L. aut Park, B. D. aut Pasqualini, L. aut Pastore, A. aut Patrizii, L. aut Pessard, H. aut Podgrudkov, D. aut Polukhina, N. aut Pozzato, M. aut Pupilli, F. aut Roda, M. aut Roganova, T. aut Rokujo, H. aut Rosa, G. aut Ryazhskaya, O. aut Sato, O. aut Schembri, A. aut Shakiryanova, I. aut Shchedrina, T. aut Shibuya, H. aut Shibayama, E. aut Shiraishi, T. aut Simone, S. aut Sirignano, C. aut Sirri, G. aut Sotnikov, A. aut Spinetti, M. aut Stanco, L. aut Starkov, N. aut Stellacci, S. M. aut Stipcevic, M. aut Strolin, P. aut Takahashi, S. aut Tenti, M. aut Terranova, F. aut Tioukov, V. aut Vasina, S. aut Vilain, P. aut Voevodina, E. aut Votano, L. aut Vuilleumier, J. L. aut Wilquet, G. aut Yoon, C. S. aut Enthalten in Journal of high energy physics Berlin : Springer, 1997 2018(2018), 6 vom: 27. Juni (DE-627)320910571 (DE-600)2027350-2 1029-8479 nnns volume:2018 year:2018 number:6 day:27 month:06 https://dx.doi.org/10.1007/JHEP06(2018)151 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2014 GBV_ILN_2020 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 2018 2018 6 27 06 |
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Agafonova, N. @@aut@@ Aleksandrov, A. @@aut@@ Anokhina, A. @@aut@@ Aoki, S. @@aut@@ Ariga, A. @@aut@@ Ariga, T. @@aut@@ Bertolin, A. @@aut@@ Bozza, C. @@aut@@ Brugnera, R. @@aut@@ Buonaura, A. @@aut@@ Buontempo, S. @@aut@@ Chernyavskiy, M. @@aut@@ Chukanov, A. @@aut@@ Consiglio, L. @@aut@@ D’Ambrosio, N. @@aut@@ De Lellis, G. @@aut@@ De Serio, M. @@aut@@ del Amo Sanchez, P. @@aut@@ Di Crescenzo, A. @@aut@@ Di Ferdinando, D. @@aut@@ Di Marco, N. @@aut@@ Dmitrievsky, S. @@aut@@ Dracos, M. @@aut@@ Duchesneau, D. @@aut@@ Dusini, S. @@aut@@ Dzhatdoev, T. @@aut@@ Ebert, J. @@aut@@ Ereditato, A. @@aut@@ Favier, J. @@aut@@ Fini, R. A. @@aut@@ Fornari, F. @@aut@@ Fukuda, T. @@aut@@ Galati, G. @@aut@@ Garfagnini, A. @@aut@@ Gentile, V. @@aut@@ Goldberg, J. @@aut@@ Gornushkin, Y. @@aut@@ Gorbunov, S. @@aut@@ Grella, G. @@aut@@ Guler, A. M. @@aut@@ Gustavino, C. @@aut@@ Hagner, C. @@aut@@ Hara, T. @@aut@@ Hayakawa, T. @@aut@@ Hollnagel, A. @@aut@@ Hosseini, B. @@aut@@ Ishiguro, K. @@aut@@ Iuliano, A. @@aut@@ Jakovcic, K. @@aut@@ Jollet, C. @@aut@@ Kamiscioglu, C. @@aut@@ Kamiscioglu, M. @@aut@@ Kim, S. H. @@aut@@ Kitagawa, N. @@aut@@ Klicek, B. @@aut@@ Kodama, K. @@aut@@ Komatsu, M. @@aut@@ Kose, U. @@aut@@ Kreslo, I. @@aut@@ Laudisio, F. @@aut@@ Lauria, A. @@aut@@ Ljubicic, A. @@aut@@ Longhin, A. @@aut@@ Loverre, P. @@aut@@ Malgin, A. @@aut@@ Malenica, M. @@aut@@ Mandrioli, G. @@aut@@ Matsuo, T. @@aut@@ Matveev, V. @@aut@@ Mauri, N. @@aut@@ Medinaceli, E. @@aut@@ Meisel, F. @@aut@@ Meregaglia, A. @@aut@@ Mikado, S. @@aut@@ Miyanishi, M. @@aut@@ Mizutani, F. @@aut@@ Monacelli, P. @@aut@@ Montesi, M. C. @@aut@@ Morishima, K. @@aut@@ Muciaccia, M. T. @@aut@@ Naganawa, N. @@aut@@ Naka, T. @@aut@@ Nakamura, M. @@aut@@ Nakano, T. @@aut@@ Niwa, K. @@aut@@ Okateva, N. @@aut@@ Ogawa, S. @@aut@@ Ozaki, K. @@aut@@ Paoloni, A. @@aut@@ Paparella, L. @@aut@@ Park, B. D. @@aut@@ Pasqualini, L. @@aut@@ Pastore, A. @@aut@@ Patrizii, L. @@aut@@ Pessard, H. @@aut@@ Podgrudkov, D. @@aut@@ Polukhina, N. @@aut@@ Pozzato, M. @@aut@@ Pupilli, F. @@aut@@ Roda, M. @@aut@@ Roganova, T. @@aut@@ Rokujo, H. @@aut@@ Rosa, G. @@aut@@ Ryazhskaya, O. @@aut@@ Sato, O. @@aut@@ Schembri, A. @@aut@@ Shakiryanova, I. @@aut@@ Shchedrina, T. @@aut@@ Shibuya, H. @@aut@@ Shibayama, E. @@aut@@ Shiraishi, T. @@aut@@ Simone, S. @@aut@@ Sirignano, C. @@aut@@ Sirri, G. @@aut@@ Sotnikov, A. @@aut@@ Spinetti, M. @@aut@@ Stanco, L. @@aut@@ Starkov, N. @@aut@@ Stellacci, S. M. @@aut@@ Stipcevic, M. @@aut@@ Strolin, P. @@aut@@ Takahashi, S. @@aut@@ Tenti, M. @@aut@@ Terranova, F. @@aut@@ Tioukov, V. @@aut@@ Vasina, S. @@aut@@ Vilain, P. @@aut@@ Voevodina, E. @@aut@@ Votano, L. @@aut@@ Vuilleumier, J. L. @@aut@@ Wilquet, G. @@aut@@ Yoon, C. S. @@aut@@ |
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Agafonova, N. Aleksandrov, A. Anokhina, A. Aoki, S. Ariga, A. Ariga, T. Bertolin, A. Bozza, C. Brugnera, R. Buonaura, A. Buontempo, S. Chernyavskiy, 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. Dmitrievsky, S. Dracos, M. Duchesneau, D. Dusini, S. Dzhatdoev, T. Ebert, J. Ereditato, A. Favier, J. Fini, R. A. Fornari, F. Fukuda, T. Galati, G. Garfagnini, A. Gentile, V. Goldberg, J. Gornushkin, Y. Gorbunov, S. Grella, G. Guler, A. M. Gustavino, C. Hagner, C. Hara, T. Hayakawa, T. Hollnagel, A. Hosseini, B. Ishiguro, K. Iuliano, A. Jakovcic, K. Jollet, C. Kamiscioglu, C. Kamiscioglu, M. Kim, S. H. Kitagawa, N. Klicek, B. Kodama, K. Komatsu, M. Kose, U. Kreslo, I. Laudisio, F. Lauria, A. Ljubicic, A. Longhin, A. Loverre, P. Malgin, A. Malenica, M. Mandrioli, G. Matsuo, T. Matveev, V. Mauri, N. Medinaceli, E. Meisel, F. Meregaglia, A. Mikado, S. Miyanishi, M. Mizutani, F. Monacelli, P. Montesi, M. C. Morishima, K. Muciaccia, M. T. Naganawa, N. Naka, T. Nakamura, M. Nakano, T. Niwa, K. Okateva, N. Ogawa, S. Ozaki, K. Paoloni, A. Paparella, L. Park, B. D. Pasqualini, L. Pastore, A. Patrizii, L. Pessard, H. Podgrudkov, D. Polukhina, N. Pozzato, M. Pupilli, F. Roda, M. Roganova, T. Rokujo, H. Rosa, G. Ryazhskaya, O. Sato, O. Schembri, A. Shakiryanova, I. Shchedrina, T. Shibuya, H. Shibayama, E. Shiraishi, T. Simone, S. Sirignano, C. Sirri, G. Sotnikov, A. Spinetti, M. Stanco, L. Starkov, N. Stellacci, S. M. Stipcevic, M. Strolin, P. Takahashi, S. Tenti, M. Terranova, F. Tioukov, V. Vasina, S. Vilain, P. Voevodina, E. Votano, L. Vuilleumier, J. L. Wilquet, G. Yoon, C. S. |
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10.1007/JHEP06(2018)151 |
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final results of the search for νμ → νe oscillations with the opera detector in the cngs beam |
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Final results of the search for νμ → νe oscillations with the OPERA detector in the CNGS beam |
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Abstract The OPERA experiment has discovered the tau neutrino appearance in the CNGS muon neutrino beam, in agreement with the 3 neutrino flavour oscillation hypothesis. The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electromagnetic showers. Moreover, thanks to the very high granularity of the emulsion films, showers induced by electrons can be distinguished from those induced by π0s, thus allowing the detection of charged current interactions of electron neutrinos. In this paper the results of the search for electron neutrino events using the full dataset are reported. An improved method for the electron neutrino energy estimation is exploited. Data are compatible with the 3 neutrino flavour mixing model expectations and are used to set limits on the oscillation parameters of the 3+1 neutrino mixing model, in which an additional mass eigenstate m4 is introduced. At high Δm412 (≳0.1 $ eV^{2} $), an upper limit on $ sin^{2} $ 2θμe is set to 0.021 at 90% C.L. and Δm412 ≳ 4 × $ 10^{− 3} $ $ eV^{2} $ is excluded for maximal mixing in appearance mode. © The Author(s) 2018 |
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Abstract The OPERA experiment has discovered the tau neutrino appearance in the CNGS muon neutrino beam, in agreement with the 3 neutrino flavour oscillation hypothesis. The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electromagnetic showers. Moreover, thanks to the very high granularity of the emulsion films, showers induced by electrons can be distinguished from those induced by π0s, thus allowing the detection of charged current interactions of electron neutrinos. In this paper the results of the search for electron neutrino events using the full dataset are reported. An improved method for the electron neutrino energy estimation is exploited. Data are compatible with the 3 neutrino flavour mixing model expectations and are used to set limits on the oscillation parameters of the 3+1 neutrino mixing model, in which an additional mass eigenstate m4 is introduced. At high Δm412 (≳0.1 $ eV^{2} $), an upper limit on $ sin^{2} $ 2θμe is set to 0.021 at 90% C.L. and Δm412 ≳ 4 × $ 10^{− 3} $ $ eV^{2} $ is excluded for maximal mixing in appearance mode. © The Author(s) 2018 |
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Abstract The OPERA experiment has discovered the tau neutrino appearance in the CNGS muon neutrino beam, in agreement with the 3 neutrino flavour oscillation hypothesis. The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electromagnetic showers. Moreover, thanks to the very high granularity of the emulsion films, showers induced by electrons can be distinguished from those induced by π0s, thus allowing the detection of charged current interactions of electron neutrinos. In this paper the results of the search for electron neutrino events using the full dataset are reported. An improved method for the electron neutrino energy estimation is exploited. Data are compatible with the 3 neutrino flavour mixing model expectations and are used to set limits on the oscillation parameters of the 3+1 neutrino mixing model, in which an additional mass eigenstate m4 is introduced. At high Δm412 (≳0.1 $ eV^{2} $), an upper limit on $ sin^{2} $ 2θμe is set to 0.021 at 90% C.L. and Δm412 ≳ 4 × $ 10^{− 3} $ $ eV^{2} $ is excluded for maximal mixing in appearance mode. © The Author(s) 2018 |
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The OPERA neutrino interaction target, made of Emulsion Cloud Chambers, was particularly efficient in the reconstruction of electromagnetic showers. Moreover, thanks to the very high granularity of the emulsion films, showers induced by electrons can be distinguished from those induced by π0s, thus allowing the detection of charged current interactions of electron neutrinos. In this paper the results of the search for electron neutrino events using the full dataset are reported. An improved method for the electron neutrino energy estimation is exploited. Data are compatible with the 3 neutrino flavour mixing model expectations and are used to set limits on the oscillation parameters of the 3+1 neutrino mixing model, in which an additional mass eigenstate m4 is introduced. 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| score |
7.3997726 |