Measurement of CNGS muon neutrino speed with Borexino

Sanchez, P. Alvarez; Barzaghi, Riccardo; Bellini, G.; Benziger, J.; Betti, B.; Biagi, L.; Bick, D.; Bonfini, G.; Bravo, D.; Avanzini, M. Buizza; Caccianiga, B.; Cadonati, L.; Carraro, C.; Cavalcante, P.; Cerretto, Giancarlo; Chavarría, Á.; D’Angelo, D.; Davini, S.; Gaetani, Carlo Iapige De; Derbin, A.; Etenko, A.; Esteban, H.; Fomenko, K.; Franco, D.; Galbiati, C.; Gazzana, S.; Ghiano, C.; Giammarchi, M.; Goeger-Neff, M.; Goretti, A.; Grandi, L.; Guardincerri, E.; Hardy, S.; Ianni, Aldo; Ianni, Andrea; Jones, M.; Kayunov, A.; Kobychev, V.; Korablëv, D.; Korga, G.; Koshio, Y.; Kryn, D.; Laubenstein, M.; Lewke, T.; Litvinovich, E.; Loer, B.; Lombardi, P.; Lombardi, F.; Ludhová, L.; Machulin, I.; Manecki, S.; Maneschg, W.; Manuzio, G.; Meindl, Q.; Meroni, E.; Miramonti, L.; Misiaszek, M.; Missiaen, D.; Montanari, D.; Mosteiro, P.; Muratova, V.; Oberauer, L.; Obolensky, M.; Ortica, F.; Otis, K.; Pallavicini, M.; Papp, L.; Passoni, D.; Pinto, Livio; Perasso, L.; Perasso, S.; Pettiti, V.; Plantard, C.; Pocar, A.; Raghavan, R. S.; Ranucci, G.; Razeto, A.; Re, A.; Romani, A.; Rossi, N.; Sabelnikov, A.; Saldanha, R.; Salvo, C.; Schöenert, S.; Serrano, J.; Simgen, H.; Skorokhvatov, M.; Smirnov, O.; Sotnikov, A.; Spinnato, P.F.; Sukhotin, S.; Suvorov, Y.; Tartaglia, R.; Testera, G.; Vignaud, D.; Visconti, M. G.; Vogelaar, R. B.; Feilitzsch, F. von; Winter, J.; Wójcik, Marcin; Wright, A.; Wurm, M.; Xu, J.; Zaimidoroga, O.; Zavatarelli, S.; Zuzel, G.

doi:10.1016/j.physletb.2012.08.052

Cited by 36 publications

(8 citation statements)

References 21 publications

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“…Although geoneutrinos can be measured, in principle, anywhere on the Earth, the experiments need to be carried out in underground (or underwater) laboratories in order to shield detectors from cosmic radiation; only a few locations therefore have particular experimental interest. We have calculated the fluxes at 16 sites where the exploration of the Earth through geoneutrinos is either currently underway (Kamioka, Japan, with the KamLAND experiment [ Araki et al ., ; Gando et al ., , ]; Gran Sasso, Italy, with the Borexino experiment [ Alvarez Sanchez et al ., ]; Sudbury, Ontario, Canada, with the SNO + experiment [ Chen , ]), or where such experiments have been proposed or could be planned (Table ). Hawaii (Hanohano) [ Dye , ], Baksan (Baksan Neutrino Observatory) [ Buklerskii et al ., ], Homestake (Deep Underground Science and Engineering Laboratory) [ Tolich et al ., ], Curacao (Earth AntineutRino Tomography) [ De Meijer et al ., ], and Daya Bay (Daya Bay II) [ Wang , ] are all sites that have been proposed for constructing liquid scintillator detectors capable of detecting geoneutrinos.…”

Section: Methodology and Reference Statesmentioning

confidence: 99%

A reference Earth model for the heat‐producing elements and associated geoneutrino flux

Huang

Chubakov

Mantovani

et al. 2013

Geochem Geophys Geosyst

187

345

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[1] The recent geoneutrino experimental results from KamLAND (Kamioka Liquid Scintillator Antineutrino Detector) and Borexino detectors reveal the usefulness of analyzing the Earth's geoneutrino flux, as it provides a constraint on the strength of the radiogenic heat power, and this, in turn, provides a test of compositional models of the bulk silicate Earth (BSE). This flux is dependent on the amount and distribution of heat-producing elements (HPEs: U, Th, and K) in the Earth's interior. We have developed a geophysically based, three-dimensional global reference model for the abundances and distributions of HPEs in the BSE. The structure and composition of the outermost portion of the Earth, the crust and underlying lithospheric mantle, are detailed in the reference model; this portion of the Earth has the greatest influence on the geoneutrino fluxes. The reference model combines three existing geophysical models of the global crust and yields an average crustal thickness of 34.4 AE 4.1 km in the continents and 8.0 AE 2.7 km in the oceans, and a total mass (in 10 22 kg) of oceanic, continental, and bulk crust is 0.67 AE 0.23, 2.06 AE 0.25, and 2.73 AE 0.48, respectively. In situ seismic velocity provided by CRUST 2.0 allows us to estimate the average composition of the deep continental crust by using new and updated compositional databases for amphibolite and granulite facies rocks in combination with laboratory ultrasonic velocities measurements. An updated xenolithic peridotite database is used to represent the average composition of continental lithospheric mantle. Monte Carlo simulation is used to predict the geoneutrino flux at 16 selected locations ©2013. American Geophysical Union. All Rights Reserved. 2003 and to track the asymmetrical uncertainties of radiogenic heat power due to the log-normal distributions of HPE concentrations in crustal rocks.

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Section: Methodology and Reference Statesmentioning

confidence: 99%

A reference Earth model for the heat‐producing elements and associated geoneutrino flux

Huang

Chubakov

Mantovani

et al. 2013

Geochem Geophys Geosyst

187

345

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“…The ICARUS result on 2011 data has been confirmed with improved precision by the other LNGS experiments [6,7] in the 2012 CNGS bunched beam campaign. We hereby report the experimental measurements of the neutrino velocity with the ICARUS detector, obtained combining the accurate determination of the distance and time of flight with the direct observation of either neutrino events inside the detector or neutrino associated muons from the surrounding rock.…”

Section: Indroductionmentioning

confidence: 58%

Precision measurement of the neutrino velocity with the ICARUS detector in the CNGS beam

Antonello¹,

Baibussinov²,

Benetti³

et al. 2012

J. High Energ. Phys.

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During May 2012, the CERN-CNGS neutrino beam has been operated for two weeks for a total of ∼ 1.8 × 10 17 p.o.t., with the proton beam made of bunches, few ns wide and separated by 100 ns. This beam structure allows a very accurate time of flight measurement of neutrinos from CERN to LNGS on an event-by-event basis.Both the ICARUS-T600 PMT-DAQ and the CERN-LNGS timing synchronization have been substantially improved for this campaign, taking advantage of additional independent GPS receivers, both at CERN and LNGS as well as of the deployment of the "White Rabbit" protocol both at CERN and LNGS.The ICARUS-T600 detector has collected 25 beam-associated events; the corresponding time of flight has been accurately evaluated, using all different time synchronization paths.The measured neutrino time of flight is compatible with the arrival of all events with speed equivalent to the one of light: the difference between the expected value based on the speed of light and the measured value is δt = tof c −tof ν = 0.10±0.67 stat. ±2.39 syst. ns. This result is in agreement with the value previously reported by the ICARUS Collaboration, δt = 0.3 ± 4.9 stat. ± 9.0 syst. ns, but with improved statistical and systematic accuracy.

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“…In parallel, this measurement also set the strongest available limit on CNO neutrinos at <7.7·10 8 cm −2 s −1 at 95% c.l., since an integrated neutrino signal between 1.0 and 1.5 MeV was measured for this result. 7 Be neutrinos The flagship Borexino result, this was also the first direct detection of this particular solar neutrino spectral component. The most recent published result [11] has a ∼5% precision for an MSW-LMA flux of (3.10±0.15)·10 9 cm −2 s −1 (Borexino rate: 46.0±1.5(stat)±1.5(sys) cpd/100 ton).…”

Section: Solar Geoneutrino and Other Resultsmentioning

confidence: 77%

“…The 7 Be signal was also used for the seasonal modulation study [14] and the verification of the LMA prediction for the lack of diurnal/nocturnal asymmetry [13] in the solar neutrino flux reaching a detector on the surface of Earth (A d−n = 0.001 ± 0.012(stat) ± 0.007(sys) cm −2 s −1 ). The Inverse Beta Decay (IBD) reaction ν e + p + → n 0 + e + is Borexino's main channel to detect antineutrino signals, of which reactor and geo-neutrinos are the most abundant example.…”

Section: Pos(hql 2016)006mentioning

confidence: 99%

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The Borexino & SOX experiments

Bravo¹,

Borexino²

2017

Proceedings of XIII International Conference on Heavy Quarks and Leptons — PoS(HQL 2016)

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Building upon its highly successful Phase I (2007)(2008)(2009)(2010) results -which demonstrated the unprecedented radiopurity and precision levels reached, through the measurement of all but two of the solar neutrino components-the Borexino neutrino observatory is producing new measurements with its Phase II (2012-present day) dataset, started after very successful calibration (2009-10) and scintillator purification (2010-11) campaigns. A new geo-neutrino flux measurement, and searches for electric charge conservation violation and GRB-correlated neutrino events lead the way in a path that will see a unified, wideband solar neutrino spectroscopy analysis with the more radiopure Phase II statistics and new data selection techniques. Furthermore, the recently-completed Borexino Thermal Management and Monitoring System (BTMMS) represents a critical detector hardware upgrade which, together with complementary numerical fluidodynamic simulations, enables us to keep watch and correct temperature excursions. At the extremely low levels of background concentration currently seen in the Fiducial Volume (FV), these may otherwise have yielded problematic fluid mixing from less radiopure, peripheral scintillator areas. Finally, a new detector-wide calibration campaign is in its final stages of preparation, just ahead of the transition to the SOX program, which will see the deployment of a ∼150 kCi 144 Ce-144 Pr source in a pit under the detector, with the aim of studying anomalous short-distance ν e oscillation effects starting in 2018.

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Measurement of CNGS muon neutrino speed with Borexino

Cited by 36 publications

References 21 publications

A reference Earth model for the heat‐producing elements and associated geoneutrino flux

A reference Earth model for the heat‐producing elements and associated geoneutrino flux

Precision measurement of the neutrino velocity with the ICARUS detector in the CNGS beam

The Borexino & SOX experiments

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