Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors
Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Agafonova, N. Yu. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2012 |
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| Schlagwörter: |
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| Anmerkung: |
© Società Italiana di Fisica and Springer 2012 |
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| Übergeordnetes Werk: |
Enthalten in: The European physical journal - Berlin : Springer, 2011, 127(2012), 6 vom: 29. Juni |
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| Übergeordnetes Werk: |
volume:127 ; year:2012 ; number:6 ; day:29 ; month:06 |
| Links: |
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| DOI / URN: |
10.1140/epjp/i2012-12071-5 |
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| Katalog-ID: |
SPR03145044X |
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| 041 | |a eng | ||
| 100 | 1 | |a Agafonova, N. Yu. |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors |
| 264 | 1 | |c 2012 | |
| 336 | |a Text |b txt |2 rdacontent | ||
| 337 | |a Computermedien |b c |2 rdamedia | ||
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| 500 | |a © Società Italiana di Fisica and Springer 2012 | ||
| 520 | |a Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos are produced and detected, respectively. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ∼ 160 m, allows the use of very high-energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique, which, as stated above, is totally independent of the TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called “Teramo anomaly”, a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m.w.e. thickness for horizontal directions. The “abundant” high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence between the two experiments correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic-horizontal-muon events and shows the existence of a negative time-shift in the OPERA set-up of the order of ΔtAB = −(73 ± 9) when two calendar periods, A and B, are compared. The first, A, goes from August 2007 to August 2008 plus the period from January 2012 to March 2012; the second period, B, goes from August 2008 to December 2011. This result shows a systematic effect in the OPERA timing system present from August 2008 until December 2011. The size of the effect, in terms of the cosmic horizontal muons TOF, is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. This technology can be implemented at LNGS for a high-precision determination of TOF with the CNGS neutrino beams. If new experiments are needed for the study of neutrino velocities they must be able to detect effects an order of magnitude smaller than the value of the OPERA systematic effect. | ||
| 650 | 4 | |a Calendar Time |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Neutrino Interaction |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Large Volume Detector |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Event Display |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Opera Experiment |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Antonioli, P. |4 aut | |
| 700 | 1 | |a Ashikhmin, V. V. |4 aut | |
| 700 | 1 | |a Bari, G. |4 aut | |
| 700 | 1 | |a Bressan, E. |4 aut | |
| 700 | 1 | |a Evans, L. |4 aut | |
| 700 | 1 | |a Garbini, M. |4 aut | |
| 700 | 1 | |a Giusti, P. |4 aut | |
| 700 | 1 | |a Malguin, A. S. |4 aut | |
| 700 | 1 | |a Persiani, R. |4 aut | |
| 700 | 1 | |a Ryasny, V. G. |4 aut | |
| 700 | 1 | |a Ryazhskaya, O. G. |4 aut | |
| 700 | 1 | |a Sartorelli, G. |4 aut | |
| 700 | 1 | |a Scapparone, E. |4 aut | |
| 700 | 1 | |a Selvi, M. |4 aut | |
| 700 | 1 | |a Shakirianova, I. R. |4 aut | |
| 700 | 1 | |a Votano, L. |4 aut | |
| 700 | 1 | |a Wenniger, H. |4 aut | |
| 700 | 1 | |a Yakushev, V. F. |4 aut | |
| 700 | 1 | |a Zichichi, A. |4 aut | |
| 700 | 1 | |a Agafonova, N. |4 aut | |
| 700 | 1 | |a Alexandrov, A. |4 aut | |
| 700 | 1 | |a Bertolin, A. |4 aut | |
| 700 | 1 | |a Brugnera, R. |4 aut | |
| 700 | 1 | |a Büttner, B. |4 aut | |
| 700 | 1 | |a Chiarella, V. |4 aut | |
| 700 | 1 | |a Chukanov, A. |4 aut | |
| 700 | 1 | |a D’Ambrosio, N. |4 aut | |
| 700 | 1 | |a De Lellis, G. |4 aut | |
| 700 | 1 | |a Di Crescenzo, A. |4 aut | |
| 700 | 1 | |a Di Ferdinando, D. |4 aut | |
| 700 | 1 | |a Di Marco, N. |4 aut | |
| 700 | 1 | |a Dmitrievsky, S. |4 aut | |
| 700 | 1 | |a Dracos, M. |4 aut | |
| 700 | 1 | |a Dusini, S. |4 aut | |
| 700 | 1 | |a Ebert, J. |4 aut | |
| 700 | 1 | |a Ereditato, A. |4 aut | |
| 700 | 1 | |a Ferber, T. |4 aut | |
| 700 | 1 | |a Fini, R. A. |4 aut | |
| 700 | 1 | |a Garfagnini, A. |4 aut | |
| 700 | 1 | |a Giacomelli, G. |4 aut | |
| 700 | 1 | |a Göllnitz, C. |4 aut | |
| 700 | 1 | |a Gornushkin, Y. |4 aut | |
| 700 | 1 | |a Grianti, F. |4 aut | |
| 700 | 1 | |a Gustavino, C. |4 aut | |
| 700 | 1 | |a Hagner, C. |4 aut | |
| 700 | 1 | |a Hierholzer, M. |4 aut | |
| 700 | 1 | |a Hollnagel, A. |4 aut | |
| 700 | 1 | |a Jakovcic, K. |4 aut | |
| 700 | 1 | |a Jollet, C. |4 aut | |
| 700 | 1 | |a Klicek, B. |4 aut | |
| 700 | 1 | |a Kose, U. |4 aut | |
| 700 | 1 | |a Lenkeit, J. |4 aut | |
| 700 | 1 | |a Ljubicic, A. |4 aut | |
| 700 | 1 | |a Longhin, A. |4 aut | |
| 700 | 1 | |a Malgin, A. |4 aut | |
| 700 | 1 | |a Mandrioli, G. |4 aut | |
| 700 | 1 | |a Matveev, V. |4 aut | |
| 700 | 1 | |a Mauri, N. |4 aut | |
| 700 | 1 | |a Medinaceli, E. |4 aut | |
| 700 | 1 | |a Meregaglia, A. |4 aut | |
| 700 | 1 | |a Muciaccia, M. T. |4 aut | |
| 700 | 1 | |a Naumov, D. |4 aut | |
| 700 | 1 | |a Olshevsky, A. |4 aut | |
| 700 | 1 | |a Paoloni, A. |4 aut | |
| 700 | 1 | |a Pastore, A. |4 aut | |
| 700 | 1 | |a Patrizii, L. |4 aut | |
| 700 | 1 | |a Pozzato, M. |4 aut | |
| 700 | 1 | |a Pupilli, F. |4 aut | |
| 700 | 1 | |a Rosa, G. |4 aut | |
| 700 | 1 | |a Rostovtseva, I. |4 aut | |
| 700 | 1 | |a Russo, A. |4 aut | |
| 700 | 1 | |a Ryazhskaya, O. |4 aut | |
| 700 | 1 | |a Schembri, A. |4 aut | |
| 700 | 1 | |a Shakirianova, I. |4 aut | |
| 700 | 1 | |a Sheshukov, A. |4 aut | |
| 700 | 1 | |a Simone, S. |4 aut | |
| 700 | 1 | |a Sioli, M. |4 aut | |
| 700 | 1 | |a Sirignano, C. |4 aut | |
| 700 | 1 | |a Sirri, G. |4 aut | |
| 700 | 1 | |a Spinetti, M. |4 aut | |
| 700 | 1 | |a Stanco, L. |4 aut | |
| 700 | 1 | |a Stipcevic, M. |4 aut | |
| 700 | 1 | |a Tenti, M. |4 aut | |
| 700 | 1 | |a Terranova, F. |4 aut | |
| 700 | 1 | |a Tioukov, V. |4 aut | |
| 700 | 1 | |a Votano, L. |4 aut | |
| 700 | 1 | |a Wonsak, B. |4 aut | |
| 700 | 1 | |a Yakushev, V. |4 aut | |
| 700 | 1 | |a Zaitsev, Y. |4 aut | |
| 700 | 1 | |a Zemskova, S. |4 aut | |
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10.1140/epjp/i2012-12071-5 doi (DE-627)SPR03145044X (SPR)i2012-12071-5-e DE-627 ger DE-627 rakwb eng Agafonova, N. Yu. verfasserin aut Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors 2012 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Società Italiana di Fisica and Springer 2012 Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos are produced and detected, respectively. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ∼ 160 m, allows the use of very high-energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique, which, as stated above, is totally independent of the TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called “Teramo anomaly”, a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m.w.e. thickness for horizontal directions. The “abundant” high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence between the two experiments correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic-horizontal-muon events and shows the existence of a negative time-shift in the OPERA set-up of the order of ΔtAB = −(73 ± 9) when two calendar periods, A and B, are compared. The first, A, goes from August 2007 to August 2008 plus the period from January 2012 to March 2012; the second period, B, goes from August 2008 to December 2011. This result shows a systematic effect in the OPERA timing system present from August 2008 until December 2011. The size of the effect, in terms of the cosmic horizontal muons TOF, is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. This technology can be implemented at LNGS for a high-precision determination of TOF with the CNGS neutrino beams. If new experiments are needed for the study of neutrino velocities they must be able to detect effects an order of magnitude smaller than the value of the OPERA systematic effect. Calendar Time (dpeaa)DE-He213 Neutrino Interaction (dpeaa)DE-He213 Large Volume Detector (dpeaa)DE-He213 Event Display (dpeaa)DE-He213 Opera Experiment (dpeaa)DE-He213 Antonioli, P. aut Ashikhmin, V. V. aut Bari, G. aut Bressan, E. aut Evans, L. aut Garbini, M. aut Giusti, P. aut Malguin, A. S. aut Persiani, R. aut Ryasny, V. G. aut Ryazhskaya, O. G. aut Sartorelli, G. aut Scapparone, E. aut Selvi, M. aut Shakirianova, I. R. aut Votano, L. aut Wenniger, H. aut Yakushev, V. F. aut Zichichi, A. aut Agafonova, N. aut Alexandrov, A. aut Bertolin, A. aut Brugnera, R. aut Büttner, B. aut Chiarella, V. aut Chukanov, A. aut D’Ambrosio, N. aut De Lellis, G. aut Di Crescenzo, A. aut Di Ferdinando, D. aut Di Marco, N. aut Dmitrievsky, S. aut Dracos, M. aut Dusini, S. aut Ebert, J. aut Ereditato, A. aut Ferber, T. aut Fini, R. A. aut Garfagnini, A. aut Giacomelli, G. aut Göllnitz, C. aut Gornushkin, Y. aut Grianti, F. aut Gustavino, C. aut Hagner, C. aut Hierholzer, M. aut Hollnagel, A. aut Jakovcic, K. aut Jollet, C. aut Klicek, B. aut Kose, U. aut Lenkeit, J. aut Ljubicic, A. aut Longhin, A. aut Malgin, A. aut Mandrioli, G. aut Matveev, V. aut Mauri, N. aut Medinaceli, E. aut Meregaglia, A. aut Muciaccia, M. T. aut Naumov, D. aut Olshevsky, A. aut Paoloni, A. aut Pastore, A. aut Patrizii, L. aut Pozzato, M. aut Pupilli, F. aut Rosa, G. aut Rostovtseva, I. aut Russo, A. aut Ryazhskaya, O. aut Schembri, A. aut Shakirianova, I. aut Sheshukov, A. aut Simone, S. aut Sioli, M. aut Sirignano, C. aut Sirri, G. aut Spinetti, M. aut Stanco, L. aut Stipcevic, M. aut Tenti, M. aut Terranova, F. aut Tioukov, V. aut Votano, L. aut Wonsak, B. aut Yakushev, V. aut Zaitsev, Y. aut Zemskova, S. aut Enthalten in The European physical journal Berlin : Springer, 2011 127(2012), 6 vom: 29. Juni (DE-627)647653958 (DE-600)2595693-0 2190-5444 nnns volume:127 year:2012 number:6 day:29 month:06 https://dx.doi.org/10.1140/epjp/i2012-12071-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 127 2012 6 29 06 |
| spelling |
10.1140/epjp/i2012-12071-5 doi (DE-627)SPR03145044X (SPR)i2012-12071-5-e DE-627 ger DE-627 rakwb eng Agafonova, N. Yu. verfasserin aut Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors 2012 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Società Italiana di Fisica and Springer 2012 Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos are produced and detected, respectively. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ∼ 160 m, allows the use of very high-energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique, which, as stated above, is totally independent of the TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called “Teramo anomaly”, a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m.w.e. thickness for horizontal directions. The “abundant” high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence between the two experiments correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic-horizontal-muon events and shows the existence of a negative time-shift in the OPERA set-up of the order of ΔtAB = −(73 ± 9) when two calendar periods, A and B, are compared. The first, A, goes from August 2007 to August 2008 plus the period from January 2012 to March 2012; the second period, B, goes from August 2008 to December 2011. This result shows a systematic effect in the OPERA timing system present from August 2008 until December 2011. The size of the effect, in terms of the cosmic horizontal muons TOF, is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. This technology can be implemented at LNGS for a high-precision determination of TOF with the CNGS neutrino beams. If new experiments are needed for the study of neutrino velocities they must be able to detect effects an order of magnitude smaller than the value of the OPERA systematic effect. Calendar Time (dpeaa)DE-He213 Neutrino Interaction (dpeaa)DE-He213 Large Volume Detector (dpeaa)DE-He213 Event Display (dpeaa)DE-He213 Opera Experiment (dpeaa)DE-He213 Antonioli, P. aut Ashikhmin, V. V. aut Bari, G. aut Bressan, E. aut Evans, L. aut Garbini, M. aut Giusti, P. aut Malguin, A. S. aut Persiani, R. aut Ryasny, V. G. aut Ryazhskaya, O. G. aut Sartorelli, G. aut Scapparone, E. aut Selvi, M. aut Shakirianova, I. R. aut Votano, L. aut Wenniger, H. aut Yakushev, V. F. aut Zichichi, A. aut Agafonova, N. aut Alexandrov, A. aut Bertolin, A. aut Brugnera, R. aut Büttner, B. aut Chiarella, V. aut Chukanov, A. aut D’Ambrosio, N. aut De Lellis, G. aut Di Crescenzo, A. aut Di Ferdinando, D. aut Di Marco, N. aut Dmitrievsky, S. aut Dracos, M. aut Dusini, S. aut Ebert, J. aut Ereditato, A. aut Ferber, T. aut Fini, R. A. aut Garfagnini, A. aut Giacomelli, G. aut Göllnitz, C. aut Gornushkin, Y. aut Grianti, F. aut Gustavino, C. aut Hagner, C. aut Hierholzer, M. aut Hollnagel, A. aut Jakovcic, K. aut Jollet, C. aut Klicek, B. aut Kose, U. aut Lenkeit, J. aut Ljubicic, A. aut Longhin, A. aut Malgin, A. aut Mandrioli, G. aut Matveev, V. aut Mauri, N. aut Medinaceli, E. aut Meregaglia, A. aut Muciaccia, M. T. aut Naumov, D. aut Olshevsky, A. aut Paoloni, A. aut Pastore, A. aut Patrizii, L. aut Pozzato, M. aut Pupilli, F. aut Rosa, G. aut Rostovtseva, I. aut Russo, A. aut Ryazhskaya, O. aut Schembri, A. aut Shakirianova, I. aut Sheshukov, A. aut Simone, S. aut Sioli, M. aut Sirignano, C. aut Sirri, G. aut Spinetti, M. aut Stanco, L. aut Stipcevic, M. aut Tenti, M. aut Terranova, F. aut Tioukov, V. aut Votano, L. aut Wonsak, B. aut Yakushev, V. aut Zaitsev, Y. aut Zemskova, S. aut Enthalten in The European physical journal Berlin : Springer, 2011 127(2012), 6 vom: 29. Juni (DE-627)647653958 (DE-600)2595693-0 2190-5444 nnns volume:127 year:2012 number:6 day:29 month:06 https://dx.doi.org/10.1140/epjp/i2012-12071-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 127 2012 6 29 06 |
| allfields_unstemmed |
10.1140/epjp/i2012-12071-5 doi (DE-627)SPR03145044X (SPR)i2012-12071-5-e DE-627 ger DE-627 rakwb eng Agafonova, N. Yu. verfasserin aut Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors 2012 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Società Italiana di Fisica and Springer 2012 Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos are produced and detected, respectively. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ∼ 160 m, allows the use of very high-energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique, which, as stated above, is totally independent of the TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called “Teramo anomaly”, a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m.w.e. thickness for horizontal directions. The “abundant” high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence between the two experiments correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic-horizontal-muon events and shows the existence of a negative time-shift in the OPERA set-up of the order of ΔtAB = −(73 ± 9) when two calendar periods, A and B, are compared. The first, A, goes from August 2007 to August 2008 plus the period from January 2012 to March 2012; the second period, B, goes from August 2008 to December 2011. This result shows a systematic effect in the OPERA timing system present from August 2008 until December 2011. The size of the effect, in terms of the cosmic horizontal muons TOF, is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. This technology can be implemented at LNGS for a high-precision determination of TOF with the CNGS neutrino beams. If new experiments are needed for the study of neutrino velocities they must be able to detect effects an order of magnitude smaller than the value of the OPERA systematic effect. Calendar Time (dpeaa)DE-He213 Neutrino Interaction (dpeaa)DE-He213 Large Volume Detector (dpeaa)DE-He213 Event Display (dpeaa)DE-He213 Opera Experiment (dpeaa)DE-He213 Antonioli, P. aut Ashikhmin, V. V. aut Bari, G. aut Bressan, E. aut Evans, L. aut Garbini, M. aut Giusti, P. aut Malguin, A. S. aut Persiani, R. aut Ryasny, V. G. aut Ryazhskaya, O. G. aut Sartorelli, G. aut Scapparone, E. aut Selvi, M. aut Shakirianova, I. R. aut Votano, L. aut Wenniger, H. aut Yakushev, V. F. aut Zichichi, A. aut Agafonova, N. aut Alexandrov, A. aut Bertolin, A. aut Brugnera, R. aut Büttner, B. aut Chiarella, V. aut Chukanov, A. aut D’Ambrosio, N. aut De Lellis, G. aut Di Crescenzo, A. aut Di Ferdinando, D. aut Di Marco, N. aut Dmitrievsky, S. aut Dracos, M. aut Dusini, S. aut Ebert, J. aut Ereditato, A. aut Ferber, T. aut Fini, R. A. aut Garfagnini, A. aut Giacomelli, G. aut Göllnitz, C. aut Gornushkin, Y. aut Grianti, F. aut Gustavino, C. aut Hagner, C. aut Hierholzer, M. aut Hollnagel, A. aut Jakovcic, K. aut Jollet, C. aut Klicek, B. aut Kose, U. aut Lenkeit, J. aut Ljubicic, A. aut Longhin, A. aut Malgin, A. aut Mandrioli, G. aut Matveev, V. aut Mauri, N. aut Medinaceli, E. aut Meregaglia, A. aut Muciaccia, M. T. aut Naumov, D. aut Olshevsky, A. aut Paoloni, A. aut Pastore, A. aut Patrizii, L. aut Pozzato, M. aut Pupilli, F. aut Rosa, G. aut Rostovtseva, I. aut Russo, A. aut Ryazhskaya, O. aut Schembri, A. aut Shakirianova, I. aut Sheshukov, A. aut Simone, S. aut Sioli, M. aut Sirignano, C. aut Sirri, G. aut Spinetti, M. aut Stanco, L. aut Stipcevic, M. aut Tenti, M. aut Terranova, F. aut Tioukov, V. aut Votano, L. aut Wonsak, B. aut Yakushev, V. aut Zaitsev, Y. aut Zemskova, S. aut Enthalten in The European physical journal Berlin : Springer, 2011 127(2012), 6 vom: 29. Juni (DE-627)647653958 (DE-600)2595693-0 2190-5444 nnns volume:127 year:2012 number:6 day:29 month:06 https://dx.doi.org/10.1140/epjp/i2012-12071-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 127 2012 6 29 06 |
| allfieldsGer |
10.1140/epjp/i2012-12071-5 doi (DE-627)SPR03145044X (SPR)i2012-12071-5-e DE-627 ger DE-627 rakwb eng Agafonova, N. Yu. verfasserin aut Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors 2012 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Società Italiana di Fisica and Springer 2012 Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos are produced and detected, respectively. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ∼ 160 m, allows the use of very high-energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique, which, as stated above, is totally independent of the TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called “Teramo anomaly”, a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m.w.e. thickness for horizontal directions. The “abundant” high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence between the two experiments correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic-horizontal-muon events and shows the existence of a negative time-shift in the OPERA set-up of the order of ΔtAB = −(73 ± 9) when two calendar periods, A and B, are compared. The first, A, goes from August 2007 to August 2008 plus the period from January 2012 to March 2012; the second period, B, goes from August 2008 to December 2011. This result shows a systematic effect in the OPERA timing system present from August 2008 until December 2011. The size of the effect, in terms of the cosmic horizontal muons TOF, is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. This technology can be implemented at LNGS for a high-precision determination of TOF with the CNGS neutrino beams. If new experiments are needed for the study of neutrino velocities they must be able to detect effects an order of magnitude smaller than the value of the OPERA systematic effect. Calendar Time (dpeaa)DE-He213 Neutrino Interaction (dpeaa)DE-He213 Large Volume Detector (dpeaa)DE-He213 Event Display (dpeaa)DE-He213 Opera Experiment (dpeaa)DE-He213 Antonioli, P. aut Ashikhmin, V. V. aut Bari, G. aut Bressan, E. aut Evans, L. aut Garbini, M. aut Giusti, P. aut Malguin, A. S. aut Persiani, R. aut Ryasny, V. G. aut Ryazhskaya, O. G. aut Sartorelli, G. aut Scapparone, E. aut Selvi, M. aut Shakirianova, I. R. aut Votano, L. aut Wenniger, H. aut Yakushev, V. F. aut Zichichi, A. aut Agafonova, N. aut Alexandrov, A. aut Bertolin, A. aut Brugnera, R. aut Büttner, B. aut Chiarella, V. aut Chukanov, A. aut D’Ambrosio, N. aut De Lellis, G. aut Di Crescenzo, A. aut Di Ferdinando, D. aut Di Marco, N. aut Dmitrievsky, S. aut Dracos, M. aut Dusini, S. aut Ebert, J. aut Ereditato, A. aut Ferber, T. aut Fini, R. A. aut Garfagnini, A. aut Giacomelli, G. aut Göllnitz, C. aut Gornushkin, Y. aut Grianti, F. aut Gustavino, C. aut Hagner, C. aut Hierholzer, M. aut Hollnagel, A. aut Jakovcic, K. aut Jollet, C. aut Klicek, B. aut Kose, U. aut Lenkeit, J. aut Ljubicic, A. aut Longhin, A. aut Malgin, A. aut Mandrioli, G. aut Matveev, V. aut Mauri, N. aut Medinaceli, E. aut Meregaglia, A. aut Muciaccia, M. T. aut Naumov, D. aut Olshevsky, A. aut Paoloni, A. aut Pastore, A. aut Patrizii, L. aut Pozzato, M. aut Pupilli, F. aut Rosa, G. aut Rostovtseva, I. aut Russo, A. aut Ryazhskaya, O. aut Schembri, A. aut Shakirianova, I. aut Sheshukov, A. aut Simone, S. aut Sioli, M. aut Sirignano, C. aut Sirri, G. aut Spinetti, M. aut Stanco, L. aut Stipcevic, M. aut Tenti, M. aut Terranova, F. aut Tioukov, V. aut Votano, L. aut Wonsak, B. aut Yakushev, V. aut Zaitsev, Y. aut Zemskova, S. aut Enthalten in The European physical journal Berlin : Springer, 2011 127(2012), 6 vom: 29. Juni (DE-627)647653958 (DE-600)2595693-0 2190-5444 nnns volume:127 year:2012 number:6 day:29 month:06 https://dx.doi.org/10.1140/epjp/i2012-12071-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 127 2012 6 29 06 |
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10.1140/epjp/i2012-12071-5 doi (DE-627)SPR03145044X (SPR)i2012-12071-5-e DE-627 ger DE-627 rakwb eng Agafonova, N. Yu. verfasserin aut Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors 2012 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Società Italiana di Fisica and Springer 2012 Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos are produced and detected, respectively. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ∼ 160 m, allows the use of very high-energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique, which, as stated above, is totally independent of the TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called “Teramo anomaly”, a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m.w.e. thickness for horizontal directions. The “abundant” high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence between the two experiments correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic-horizontal-muon events and shows the existence of a negative time-shift in the OPERA set-up of the order of ΔtAB = −(73 ± 9) when two calendar periods, A and B, are compared. The first, A, goes from August 2007 to August 2008 plus the period from January 2012 to March 2012; the second period, B, goes from August 2008 to December 2011. This result shows a systematic effect in the OPERA timing system present from August 2008 until December 2011. The size of the effect, in terms of the cosmic horizontal muons TOF, is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. This technology can be implemented at LNGS for a high-precision determination of TOF with the CNGS neutrino beams. If new experiments are needed for the study of neutrino velocities they must be able to detect effects an order of magnitude smaller than the value of the OPERA systematic effect. Calendar Time (dpeaa)DE-He213 Neutrino Interaction (dpeaa)DE-He213 Large Volume Detector (dpeaa)DE-He213 Event Display (dpeaa)DE-He213 Opera Experiment (dpeaa)DE-He213 Antonioli, P. aut Ashikhmin, V. V. aut Bari, G. aut Bressan, E. aut Evans, L. aut Garbini, M. aut Giusti, P. aut Malguin, A. S. aut Persiani, R. aut Ryasny, V. G. aut Ryazhskaya, O. G. aut Sartorelli, G. aut Scapparone, E. aut Selvi, M. aut Shakirianova, I. R. aut Votano, L. aut Wenniger, H. aut Yakushev, V. F. aut Zichichi, A. aut Agafonova, N. aut Alexandrov, A. aut Bertolin, A. aut Brugnera, R. aut Büttner, B. aut Chiarella, V. aut Chukanov, A. aut D’Ambrosio, N. aut De Lellis, G. aut Di Crescenzo, A. aut Di Ferdinando, D. aut Di Marco, N. aut Dmitrievsky, S. aut Dracos, M. aut Dusini, S. aut Ebert, J. aut Ereditato, A. aut Ferber, T. aut Fini, R. A. aut Garfagnini, A. aut Giacomelli, G. aut Göllnitz, C. aut Gornushkin, Y. aut Grianti, F. aut Gustavino, C. aut Hagner, C. aut Hierholzer, M. aut Hollnagel, A. aut Jakovcic, K. aut Jollet, C. aut Klicek, B. aut Kose, U. aut Lenkeit, J. aut Ljubicic, A. aut Longhin, A. aut Malgin, A. aut Mandrioli, G. aut Matveev, V. aut Mauri, N. aut Medinaceli, E. aut Meregaglia, A. aut Muciaccia, M. T. aut Naumov, D. aut Olshevsky, A. aut Paoloni, A. aut Pastore, A. aut Patrizii, L. aut Pozzato, M. aut Pupilli, F. aut Rosa, G. aut Rostovtseva, I. aut Russo, A. aut Ryazhskaya, O. aut Schembri, A. aut Shakirianova, I. aut Sheshukov, A. aut Simone, S. aut Sioli, M. aut Sirignano, C. aut Sirri, G. aut Spinetti, M. aut Stanco, L. aut Stipcevic, M. aut Tenti, M. aut Terranova, F. aut Tioukov, V. aut Votano, L. aut Wonsak, B. aut Yakushev, V. aut Zaitsev, Y. aut Zemskova, S. aut Enthalten in The European physical journal Berlin : Springer, 2011 127(2012), 6 vom: 29. Juni (DE-627)647653958 (DE-600)2595693-0 2190-5444 nnns volume:127 year:2012 number:6 day:29 month:06 https://dx.doi.org/10.1140/epjp/i2012-12071-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 127 2012 6 29 06 |
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Agafonova, N. Yu. @@aut@@ Antonioli, P. @@aut@@ Ashikhmin, V. V. @@aut@@ Bari, G. @@aut@@ Bressan, E. @@aut@@ Evans, L. @@aut@@ Garbini, M. @@aut@@ Giusti, P. @@aut@@ Malguin, A. S. @@aut@@ Persiani, R. @@aut@@ Ryasny, V. G. @@aut@@ Ryazhskaya, O. G. @@aut@@ Sartorelli, G. @@aut@@ Scapparone, E. @@aut@@ Selvi, M. @@aut@@ Shakirianova, I. R. @@aut@@ Votano, L. @@aut@@ Wenniger, H. @@aut@@ Yakushev, V. F. @@aut@@ Zichichi, A. @@aut@@ Agafonova, N. @@aut@@ Alexandrov, A. @@aut@@ Bertolin, A. @@aut@@ Brugnera, R. @@aut@@ Büttner, B. @@aut@@ Chiarella, V. @@aut@@ Chukanov, A. @@aut@@ D’Ambrosio, N. @@aut@@ De Lellis, G. @@aut@@ Di Crescenzo, A. @@aut@@ Di Ferdinando, D. @@aut@@ Di Marco, N. @@aut@@ Dmitrievsky, S. @@aut@@ Dracos, M. @@aut@@ Dusini, S. @@aut@@ Ebert, J. @@aut@@ Ereditato, A. @@aut@@ Ferber, T. @@aut@@ Fini, R. A. @@aut@@ Garfagnini, A. @@aut@@ Giacomelli, G. @@aut@@ Göllnitz, C. @@aut@@ Gornushkin, Y. @@aut@@ Grianti, F. @@aut@@ Gustavino, C. @@aut@@ Hagner, C. @@aut@@ Hierholzer, M. @@aut@@ Hollnagel, A. @@aut@@ Jakovcic, K. @@aut@@ Jollet, C. @@aut@@ Klicek, B. @@aut@@ Kose, U. @@aut@@ Lenkeit, J. @@aut@@ Ljubicic, A. @@aut@@ Longhin, A. @@aut@@ Malgin, A. @@aut@@ Mandrioli, G. @@aut@@ Matveev, V. @@aut@@ Mauri, N. @@aut@@ Medinaceli, E. @@aut@@ Meregaglia, A. @@aut@@ Muciaccia, M. T. @@aut@@ Naumov, D. @@aut@@ Olshevsky, A. @@aut@@ Paoloni, A. @@aut@@ Pastore, A. @@aut@@ Patrizii, L. @@aut@@ Pozzato, M. @@aut@@ Pupilli, F. @@aut@@ Rosa, G. @@aut@@ Rostovtseva, I. @@aut@@ Russo, A. @@aut@@ Ryazhskaya, O. @@aut@@ Schembri, A. @@aut@@ Shakirianova, I. @@aut@@ Sheshukov, A. @@aut@@ Simone, S. @@aut@@ Sioli, M. @@aut@@ Sirignano, C. @@aut@@ Sirri, G. @@aut@@ Spinetti, M. @@aut@@ Stanco, L. @@aut@@ Stipcevic, M. @@aut@@ Tenti, M. @@aut@@ Terranova, F. @@aut@@ Tioukov, V. @@aut@@ Wonsak, B. @@aut@@ Yakushev, V. @@aut@@ Zaitsev, Y. @@aut@@ Zemskova, S. @@aut@@ |
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Agafonova, N. Yu. misc Calendar Time misc Neutrino Interaction misc Large Volume Detector misc Event Display misc Opera Experiment Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors |
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Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors Calendar Time (dpeaa)DE-He213 Neutrino Interaction (dpeaa)DE-He213 Large Volume Detector (dpeaa)DE-He213 Event Display (dpeaa)DE-He213 Opera Experiment (dpeaa)DE-He213 |
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Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors |
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Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors |
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Agafonova, N. Yu. Antonioli, P. Ashikhmin, V. V. Bari, G. Bressan, E. Evans, L. Garbini, M. Giusti, P. Malguin, A. S. Persiani, R. Ryasny, V. G. Ryazhskaya, O. G. Sartorelli, G. Scapparone, E. Selvi, M. Shakirianova, I. R. Votano, L. Wenniger, H. Yakushev, V. F. Zichichi, A. Agafonova, N. Alexandrov, A. Bertolin, A. Brugnera, R. Büttner, B. Chiarella, V. Chukanov, A. D’Ambrosio, N. De Lellis, G. Di Crescenzo, A. Di Ferdinando, D. Di Marco, N. Dmitrievsky, S. Dracos, M. Dusini, S. Ebert, J. Ereditato, A. Ferber, T. Fini, R. A. Garfagnini, A. Giacomelli, G. Göllnitz, C. Gornushkin, Y. Grianti, F. Gustavino, C. Hagner, C. Hierholzer, M. Hollnagel, A. Jakovcic, K. Jollet, C. Klicek, B. Kose, U. Lenkeit, J. Ljubicic, A. Longhin, A. Malgin, A. Mandrioli, G. Matveev, V. Mauri, N. Medinaceli, E. Meregaglia, A. Muciaccia, M. T. Naumov, D. Olshevsky, A. Paoloni, A. Pastore, A. Patrizii, L. Pozzato, M. Pupilli, F. Rosa, G. Rostovtseva, I. Russo, A. Ryazhskaya, O. Schembri, A. Shakirianova, I. Sheshukov, A. Simone, S. Sioli, M. Sirignano, C. Sirri, G. Spinetti, M. Stanco, L. Stipcevic, M. Tenti, M. Terranova, F. Tioukov, V. Wonsak, B. Yakushev, V. Zaitsev, Y. Zemskova, S. |
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determination of a time-shift in the opera set-up using high-energy horizontal muons in the lvd and opera detectors |
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Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors |
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Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos are produced and detected, respectively. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ∼ 160 m, allows the use of very high-energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique, which, as stated above, is totally independent of the TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called “Teramo anomaly”, a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m.w.e. thickness for horizontal directions. The “abundant” high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence between the two experiments correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic-horizontal-muon events and shows the existence of a negative time-shift in the OPERA set-up of the order of ΔtAB = −(73 ± 9) when two calendar periods, A and B, are compared. The first, A, goes from August 2007 to August 2008 plus the period from January 2012 to March 2012; the second period, B, goes from August 2008 to December 2011. This result shows a systematic effect in the OPERA timing system present from August 2008 until December 2011. The size of the effect, in terms of the cosmic horizontal muons TOF, is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. This technology can be implemented at LNGS for a high-precision determination of TOF with the CNGS neutrino beams. If new experiments are needed for the study of neutrino velocities they must be able to detect effects an order of magnitude smaller than the value of the OPERA systematic effect. © Società Italiana di Fisica and Springer 2012 |
| abstractGer |
Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos are produced and detected, respectively. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ∼ 160 m, allows the use of very high-energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique, which, as stated above, is totally independent of the TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called “Teramo anomaly”, a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m.w.e. thickness for horizontal directions. The “abundant” high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence between the two experiments correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic-horizontal-muon events and shows the existence of a negative time-shift in the OPERA set-up of the order of ΔtAB = −(73 ± 9) when two calendar periods, A and B, are compared. The first, A, goes from August 2007 to August 2008 plus the period from January 2012 to March 2012; the second period, B, goes from August 2008 to December 2011. This result shows a systematic effect in the OPERA timing system present from August 2008 until December 2011. The size of the effect, in terms of the cosmic horizontal muons TOF, is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. This technology can be implemented at LNGS for a high-precision determination of TOF with the CNGS neutrino beams. If new experiments are needed for the study of neutrino velocities they must be able to detect effects an order of magnitude smaller than the value of the OPERA systematic effect. © Società Italiana di Fisica and Springer 2012 |
| abstract_unstemmed |
Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos are produced and detected, respectively. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ∼ 160 m, allows the use of very high-energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique, which, as stated above, is totally independent of the TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called “Teramo anomaly”, a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m.w.e. thickness for horizontal directions. The “abundant” high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence between the two experiments correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic-horizontal-muon events and shows the existence of a negative time-shift in the OPERA set-up of the order of ΔtAB = −(73 ± 9) when two calendar periods, A and B, are compared. The first, A, goes from August 2007 to August 2008 plus the period from January 2012 to March 2012; the second period, B, goes from August 2008 to December 2011. This result shows a systematic effect in the OPERA timing system present from August 2008 until December 2011. The size of the effect, in terms of the cosmic horizontal muons TOF, is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. This technology can be implemented at LNGS for a high-precision determination of TOF with the CNGS neutrino beams. If new experiments are needed for the study of neutrino velocities they must be able to detect effects an order of magnitude smaller than the value of the OPERA systematic effect. © Società Italiana di Fisica and Springer 2012 |
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<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">SPR03145044X</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230331072716.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">201007s2012 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1140/epjp/i2012-12071-5</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)SPR03145044X</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(SPR)i2012-12071-5-e</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Agafonova, N. Yu.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Determination of a time-shift in the OPERA set-up using high-energy horizontal muons in the LVD and OPERA detectors</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2012</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">© Società Italiana di Fisica and Springer 2012</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a way totally independent of the Time-Of-Flight (TOF) measurements of CNGS neutrino events and without the need to know the distance between the two laboratories, CERN and LNGS, where the neutrinos are produced and detected, respectively. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ∼ 160 m, allows the use of very high-energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique, which, as stated above, is totally independent of the TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called “Teramo anomaly”, a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m.w.e. thickness for horizontal directions. The “abundant” high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence between the two experiments correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic-horizontal-muon events and shows the existence of a negative time-shift in the OPERA set-up of the order of ΔtAB = −(73 ± 9) when two calendar periods, A and B, are compared. The first, A, goes from August 2007 to August 2008 plus the period from January 2012 to March 2012; the second period, B, goes from August 2008 to December 2011. This result shows a systematic effect in the OPERA timing system present from August 2008 until December 2011. The size of the effect, in terms of the cosmic horizontal muons TOF, is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. This technology can be implemented at LNGS for a high-precision determination of TOF with the CNGS neutrino beams. 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| score |
7.4000425 |