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Search Results: 1 - 10 of 208474 matches for " L. Votano "
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A non-conventional neutrino beamline for the measurement of the electron neutrino cross section
A. Berra,S. Cecchini,F. Cindolo,C. Jollet,A. Longhin,L. Ludovici,G. Mandrioli,N. Mauri,A. Meregaglia,A. Paoloni,L. Pasqualini,L. Patrizii,F. Pupilli,M. Pozzato,M. Prest,G. Sirri,F. Terranova,E. Vallazza,L. Votano
Physics , 2015,
Abstract: Absolute neutrino cross section measurements at the GeV scale are ultimately limited by the knowledge of the initial $\nu$ flux. In order to evade such limitation and reach the accuracy that is needed for precision oscillation physics ($\sim 1$%), substantial advances in flux measurement techniques are requested. We discuss here the possibility of instrumenting the decay tunnel to identify large-angle positrons and monitor $\nu_e$ production from $K^+ \rightarrow e^+ \nu_e \pi^0$ decays. This non conventional technique opens up opportunities to measure the $\nu_e$ CC cross section at the per cent level in the energy range of interest for DUNE/HK. We discuss the progress in the simulation of the facility (beamline and instrumentation) and the ongoing R&D.
The OPERA magnetic spectrometer
M. Ambrosio,R. Brugnera,S. Dusini,B. Dulach,C. Fanin,G. Felici,F. Dal Corso,A. Garfagnini,F. Grianti,C. Gustavino,P. Monacelli,A. Paoloni,L. Stanco,M. Spinetti,F. Terranova,L. Votano
Physics , 2004, DOI: 10.1109/TNS.2004.829659
Abstract: The OPERA neutrino oscillation experiment foresees the construction of two magnetized iron spectrometers located after the lead-nuclear emulsion targets. The magnet is made up of two vertical walls of rectangular cross section connected by return yokes. The particle trajectories are measured by high precision drift tubes located before and after the arms of the magnet. Moreover, the magnet steel is instrumented with Resistive Plate Chambers that ease pattern recognition and allow a calorimetric measurement of the hadronic showers. In this paper we review the construction of the spectrometers. In particular, we describe the results obtained from the magnet and RPC prototypes and the installation of the final apparatus at the Gran Sasso laboratories. We discuss the mechanical and magnetic properties of the steel and the techniques employed to calibrate the field in the bulk of the magnet. Moreover, results of the tests and issues concerning the mass production of the Resistive Plate Chambers are reported. Finally, the expected physics performance of the detector is described; estimates rely on numerical simulations and the outcome of the tests described above.
CNGS beam monitor with the LVD detector
M. Aglietta,P. Antonioli,G. Bari,C. Castagnoli,W. Fulgione,P. Galeotti,M. Garbini,P. L. Ghia,P. Giusti,E. Kemp,A. S. Malguin,H. Menghetti,A. Pesci,I. A. Pless,A. Porta,V. G. Ryasny,O. G. Ryazhskaya,O. Saavedra,G. Sartorelli,M. Selvi,C. Vigorito,L. Votano,V. F. Yakushev,G. T. Zatsepin,A. Zichichi
Physics , 2003, DOI: 10.1016/j.nima.2003.07.068
Abstract: The importance of an adequate CNGS beam monitor at the Gran Sasso Laboratory has been stressed in many papers. Since the number of internal $\nu_\mu$ CC and NC interactions in the various detectors will not allow to collect statistics rapidly, one should also be able to detect the $\nu_\mu$ CC interactions in the upstream rock. In this study we have investigated the performances of the LVD detector as a monitor for the CNGS neutrino beam. Thanks to its wide area ($13 \times 11 m^2$ orthogonal to the beam direction) LVD can detect about 120 muons per day originated by $\nu_\mu$ CC interactions in the rock. The LVD total mass is $\sim2 kt$. This allows to get 30 more CNGS events per day as internal $(NC + CC)$ $\nu_\mu$ interactions, for a total of $\sim 150$ events per day. A 3% statistical error can be reached in 7 days. Taking into account the time characteristics of the CNGS beam, the cosmic muon background can be reduced to a negligible level, of the order of 1.5 events per day.
Study of Coincidences between Resonant Gravitational Wave Detectors
P. Astone,M. Bassan,P. Bonifazi,P. Carelli,E. Coccia,C. Cosmelli,S. D'Antonio,V. Fafone,G. Federici,A. Marini,Y. Minenkov,I. Modena,G. Modestino,A. Moleti,G. V. Pallottino,G. Pizzella,L. Quintieri,F. Ronga,R. Terenzi M. Visco,L. Votano
Physics , 2000, DOI: 10.1088/0264-9381/18/2/304
Abstract: Coincidences are searched with the cryogenic resonant gravitational wave detectors EXPLORER and NAUTILUS, during a period of about six months (2 June-14 December 1998) for a total measuring time of 94.5 days, with the purpose to study new algorithms of analysis, based on the physical characteristics of the detectors.
Energetic Cosmic Rays observed by the resonant gravitational wave detector NAUTILUS
P. Astone,M. Bassan,P. Bonifazi,P. Carelli,E. Coccia,S. D'Antonio,V. Fafone,G. Federici,A. Marini,G. Mazzitelli,Y. Minenkov,I. Modena,G. Modestino,A. Moleti,G. V. Pallottino,V. Pampaloni,G. Pizzella,L. Quintieri,F. Ronga,R. Terenzi,M. Visco,L. Votano
Physics , 2000, DOI: 10.1016/S0370-2693(01)00026-0
Abstract: Cosmic ray showers interacting with the resonant mass gravitational wave antenna NAUTILUS have been detected. The experimental results show large signals at a rate much greater than expected. The largest signal corresponds to an energy release in NAUTILUS of 87 TeV. We remark that a resonant mass gravitational wave detector used as particle detector has characteristics different from the usual particle detectors, and it could detect new features of cosmic rays. Among several possibilities, one can invoke unexpected behaviour of superconducting Aluminium as particle detector, producing enhanced signals, the excitation of non-elastic modes with large energy release or anomalies in cosmic rays (for instance, the showers might include exotic particles as nuclearites or Q-balls). Suggestions for explaining these observations are solicited.
Effects of neutrino oscillations on the supernova signal in LVD
M. Aglietta,P. Antonioli,G. Bari,C. Castagnoli,W. Fulgione,P. Galeotti,PL. Ghia,P. Giusti,E. Kemp,A. S. Malguin,G. Nurzia,A. Pesci,P. Picchi,I. A. Pless,V. G. Ryasny,O. G. Ryazhskaya,G. Sartorelli,M. Selvi,C. Vigorito,F. Vissani,L. Votano,V. F. Yakushev,G. T. Zatsepin,A. Zichichi
Physics , 2001, DOI: 10.1016/S0920-5632(02)01525-6
Abstract: We study the impact of neutrino oscillations on the supernova neutrino signal in the Large Volume Detector (LVD). The number of expected events for a galactic supernova (D=10 kpc) is calculated, assuming neutrino masses and mixing that explain solar and atmospheric neutrino results. The possibility to detect neutrinos in different channels makes LVD sensitive to different scenarios for neutrino properties, such as normal or inverted neutrino mass hierarchy, and/or adiabatic or non adiabatic MSW resonances associated to U(e3). Of particular importance are the charged current reactions on carbon: oscillations increase by almost one order of magnitude the number of events expected from this channel.
On-line recognition of supernova neutrino bursts in the LVD detector
Agafonova, N. Yu.;Aglietta, M.;Antonioli, P.;Bari, G.;Bonardi, A.;Boyarkin, V. V.;Bruno, G.;Fulgione, W.;Galeotti, P.;Garbini, M.;Ghia, P. L.;Giusti, P.;Gomez, F.;Kemp, E.;Kuznetsov, V. V.;Kuznetsov, V. A.;Malguin, A. S.;Menghetti, H.;Pesci, A.;Persiani, R.;Pless, I. A.;Porta, A.;Ryasny, V. G.;Ryazhskaya, O. G.;Saavedra, O.;Sartorelli, G.;Selvi, M.;Vigorito, C.;Votano, L.;Yakushev, V. F.;Zatsepin, G. T.;Zichichi, A.
High Energy Physics - Phenomenology , 2007, DOI: 10.1016/j.astropartphys.2007.09.005
Abstract: In this paper we show the capabilities of the Large Volume Detector (INFN Gran Sasso National Laboratory) to identify a neutrino burst associated to a supernova explosion, in the absence of an "external trigger", e.g., an optical observation. We describe how the detector trigger and event selection have been optimized for this purpose, and we detail the algorithm used for the on-line burst recognition. The on-line sensitivity of the detector is defined and discussed in terms of supernova distance and electron anti-neutrino intensity at the source.
First CNGS events detected by LVD
N. Yu. Agafonova,M. Aglietta,P. Antonioli,G. Bari,A. Bonardi,V. V. Boyarkin,G. Bruno,W. Fulgione,P. Galeotti,M. Garbini,P. L. Ghia,P. Giusti,E. Kemp,V. V. Kuznetsov,V. A. Kuznetsov,A. S. Malguin,H. Menghetti,R. Persiani,A. Pesci,I. A. Pless,A. Porta,V. G. Ryasny,O. G. Ryazhskaya,O. Saavedra,G. Sartorelli,M. Selvi,C. Vigorito,L. Votano,V. F. Yakushev,G. T. Zatsepin,A. Zichichi
Physics , 2007, DOI: 10.1140/epjc/s10052-007-0445-x
Abstract: The CERN Neutrino to Gran Sasso (CNGS) project aims to produce a high energy, wide band $\nu_{\mu}$ beam at CERN and send it toward the INFN Gran Sasso National Laboratory (LNGS), 732 km away. Its main goal is the observation of the $\nu_{\tau}$ appearance, through neutrino flavour oscillation. The beam started its operation in August 2006 for about 12 days: a total amount of $7.6~10^{17}$ protons were delivered to the target. The LVD detector, installed in hall A of the LNGS and mainly dedicated to the study of supernova neutrinos, was fully operating during the whole CNGS running time. A total number of 569 events were detected in coincidence with the beam spill time. This is in good agreement with the expected number of events from Montecarlo simulations.
Initial operation of the International Gravitational Event Collaboration
G. A. Prodi,I. S. Heng,Z. A. Allen,P. Astone,L. Baggio,M. Bassan,D. G. Blair,M. Bonaldi,P. Bonifazi,P. Carelli,M. Cerdonio,E. Coccia,L. Conti,C. Cosmelli,V. Crivelli Visconti,S. D'Antonio,V. Fafone,P. Falferi,P. Fortini,S. Frasca,W. O. Hamilton,E. N. Ivanov,W. W. Johnson,C. R. Locke,A. Marini,V. Martinucci,E. Mauceli,M. P. McHugh,R. Mezzena,Y. Minenkov,I. Modena,G. Modestino,A. Moleti,A. Ortolan,G. V. Pallottino,G. Pizzella,E. Rocco,F. Ronga,F. Salemi,G. Santostasi,L. Taffarello,R. Terenzi,M. E. Tobar,G. Vedovato,A. Vinante,M. Visco,S. Vitale,L. Votano,J. P. Zendri
Physics , 2000, DOI: 10.1142/S0218271800000219
Abstract: The International Gravitational Event Collaboration, IGEC, is a coordinated effort by research groups operating gravitational wave detectors working towards the detection of millisecond bursts of gravitational waves. Here we report on the current IGEC resonant bar observatory, its data analysis procedures, the main properties of the first exchanged data set. Even though the available data set is not complete, in the years 1997 and 1998 up to four detectors were operating simultaneously. Preliminary results are mentioned.
Determination of a time-shift in the OPERA set-up using high energy horizontal muons in the LVD and OPERA detectors
N. Yu. Agafonova,P. Antonioli,V. V. Ashikhmin,G. Bari,E. Bressan,L. Evans,M. Garbini,P. Giusti,A. S. Malguin,R. Persiani,V. G. Ryasny,O. G. Ryazhskaya,G. Sartorelli,E. Scapparone,M. Selvi,I. R. Shakirianova,L. Votano,H. Wenninger,V. F. Yakushev,A. Zichichi,N. Agafonova,A. Alexandrov,A. Bertolin,R. Brugnera,B. Buttner,V. Chiarella,A. Chukanov,N. D'Ambrosio,G. De Lellis,A. Di Crescenzo,D. Di Ferdinando,N. Di Marco,S. Dmitrievsky,M. Dracos,S. Dusini,J. Ebert,A. Ereditato,T. Ferber,R. A. Fini,A. Garfagnini,G. Giacomelli,C. G?llnitz,Y. Gornushkin,F. Grianti,C. Gustavino,C. Hagner,M. Hierholzer,A. Hollnagel,K. Jakovcic,C. Jollet-Meregaglia,B. Klicek,U. Kose,J. Lenkeit,A. Ljubicic,A. Longhin,A. Malgin,G. Mandrioli,V. Matveev,N. Mauri,E. Medinaceli,A. Meregaglia,M. T. Muciaccia,D. Naumov,A. Olshevsky,A. Paoloni,A. Pastore,L. Patrizii,M. Pozzato,F. Pupilli,G. Rosa,I. Rostovtseva,A. Russo,O. Ryazhskaya,A. Schembri,I. Shakirianova,A. Sheshukov,S. Simone,M. Sioli,C. Sirignano,G. Sirri,M. Spinetti,L. Stanco,M. Stipcevic,M. Tenti,F. Terranova,V. Tioukov,L. Votano,B. Wonsak,V. Yakushev,Y. Zaitsev,S. Zemskova
Physics , 2012,
Abstract: The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a totally independent way from Time Of Flight (TOF) measurements of CNGS neutrino events. 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 is totally independent from 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 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 deltaT(AB) = - (73 \pm 9) ns when two calendar periods, A and B, are compared. This result shows a systematic effect in the OPERA timing system from August 2008 until December 2011. The size of the effect 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. That technology can be implemented at LNGS for a high precision determination of TOF with the CNGS neutrino beams of an order of magnitude smaller than the value of the OPERA systematic effect.
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