Segmented Antineutrino Directional Detector (SANDD)
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Chasing the Light Sterile Neutrino Status of the STEREO Experiment
Chasing the light sterile neutrino Status of the STEREO experiment Alessandro Minotti (IRFU - CEA Saclay) on behalf of the STEREO collaboration 16/03/2017 Outlook • Neutrino physics and oscillation • Reactor neutrinos and the Reactor Antineutrino Anomaly • The STEREO experiment: principle, configuration, and timeline of the installation and commissioning phase • The STEREO experiment: status of the analysis of first collected data Alessandro Minotti (CEA - IRFU) Outlook • Neutrino physics and oscillation • Reactor neutrinos and the Reactor Antineutrino Anomaly • The STEREO experiment: principle, configuration, and timeline of the installation and commissioning phase • The STEREO experiment: status of the analysis of first collected data Neutrino Physics and Oscillation Alessandro Minotti (CEA - IRFU) The Neutrino • Neutrinos (ν) = neutral leptons - A wide range of sources and energies - Standard Model: 3 massless and only LH ν (RH ν̄) νe νμ ντ W+ e+ W+ μ+ W+ τ+ • Neutrinos oscillate (change flavour) propagating α+ β+ - Energy-dependent deficit in solar ν flux να Flavour changing νβ W+ - Distance-dependent deficit for atmospheric ν’s KOSMISK Electron-neutrinosSUN STRÅLNING are produced in the ATMOSFÄR Sun center. SUPER- KAMIOKANDE 2015 SNO Neutrino Physics and Oscillation Alessandro Minotti (CEA - IRFU) #4 Oscillation Formalism • Neutrinos oscillate (change flavour) propagating α+ β+ να Flavour changing νβ Very small but non-zero different massesAs you can see, theW oscillatory+ behaviour comes from the difference in the energy eigenvalues of ν > and ν > (E WeakE ), Hamiltonian which we interpretFree Hamiltonian as coming fromWeak di Hamiltonianfferent masses for each of themass | 1 | 2 2 − 1 + Flavour eigenstates are a mix of eigenvalues.mass eigenstates A plot of this function is shown in Figure 7 for a particular setUnitary of parameters : ∆m2 =3 10−3eV 2, (like K̄ ⁰ K⁰ and KS KL) 2 × sin (2θ)=0.8andEν =1GeV.AtL = 0, the oscillation probability is zero and the corresponding 2 L π survival probability is one. -
Radiochemical Solar Neutrino Experiments, "Successful and Otherwise"
BNL-81686-2008-CP Radiochemical Solar Neutrino Experiments, "Successful and Otherwise" R. L. Hahn Presented at the Proceedings of the Neutrino-2008 Conference Christchurch, New Zealand May 25 - 31, 2008 September 2008 Chemistry Department Brookhaven National Laboratory P.O. Box 5000 Upton, NY 11973-5000 www.bnl.gov Notice: This manuscript has been authored by employees of Brookhaven Science Associates, LLC under Contract No. DE-AC02-98CH10886 with the U.S. Department of Energy. The publisher by accepting the manuscript for publication acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. This preprint is intended for publication in a journal or proceedings. Since changes may be made before publication, it may not be cited or reproduced without the author’s permission. DISCLAIMER This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency thereof, nor any of their employees, nor any of their contractors, subcontractors, or their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or any third party’s use or the results of such use of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof or its contractors or subcontractors. -
The Analysis of the Results of the Neutrino-4 Experiment on Search for Sterile Neutrino and Comparison with Results of Other Experiments
The analysis of the results of the Neutrino-4 experiment on search for sterile neutrino and comparison with results of other experiments А.P. Serebrov, R.M. Samoilov, NRC “KI” Petersburg Nuclear Physics Institute, Gatchinа, Russia E-mail: [email protected] Abstract We present new results of measurements of reactor antineutrino flux and spectrum dependence on the distance in the range 6-12 meters from the center of the reactor core. Additional measurements were carried out and set of data to perform statistical analysis was almost doubled since the previous report. 2 Using all collected data, we performed the model independent analysis on the oscillation parameters ∆m14 2 and sin 2휃14. The method of coherent summation of results of measurements allows us to directly observe 2 the effect of oscillations. We observed an oscillation effect in vicinity of Δm14 = (7.25 ± 0.13푠푡푎푡 ± 2 2 1.08푠푦푠푡 )eV and sin 2휃 = 0.26 ± 0.08푠푡푎푡 ± 0.05푠푦푠푡. We provide a comparison of our results with results of other experiments on search for sterile neutrino. Combining the result of the Neutrino-4 experiment and the results of measurements of the gallium anomaly and reactor anomaly we obtained 2 value sin 2θ14 ≈ 0.19 ± 0.04 (4.6σ). Also was performed comparison of Neutrino-4 experimental results with results of other reactor experiments NEOS, DANSS, STEREO, PROSPECT and accelerator experiments MiniBooNE, LSND and IceCube experiment. Mass of sterile neutrino obtained from data collected in the Neutrino-4 experiment (in assumption 2 2 m4 ≈ Δm14) is m4 = 2.68 ± 0.13eV. Using the estimations of mixing angles obtained in other experiments and our new results we can calculate, within 3+1 neutrino model, masses of electron, muon, eff eff eff and tau neutrinos: m휈푒 = (0.58 ± 0.09)eV, m휈휇 = (0.42 ± 0.24)eV, m휈휏 ≤ 0.65eV. -
Searching for Lightweight Dark Matter in Nova Near Detector
Searching for Lightweight Dark Matter in NOvA Near Detector PoS(FPCP2017)056 Filip Jediný* Czech Technical University in Prague Brehova 7, Prague, Czech Republic E-mail: [email protected] Athanasios Hatzikoutelis University of Tennessee Knoxville Knoxville, TN, USA E-mail: [email protected] Sergey Kotelnikov Fermi National Accelerator Laboratory Kirk and Pine st., Batavia, IL, USA E-mail: [email protected] Biao Wang Southern Methodist University Dallas, TX, USA E-mail: [email protected] The NOvA long-baseline neutrino oscillation experiment is receiving record numbers of 120GeV protons on target from Fermilab's NuMI neutrino beam. We take advantage of our experiment’s sophisticated particle identification algorithms to search for Lightweight Dark Matter (LDM) in the first year of data from the Near Detector of NOvA (300-ton low-Z mass, placed off the beam axis) during the experiment’s first physics runs. Theoretical models of LDM predict that bellow- 10GeV candidates produced in the NuMI target might scatter or decay in the NOvA Near Detector. We simulate an example of the Neutral Vector Portal model with the sensitivity estimate of 10-39 cm2, which corresponds to O(10) LDM candidates per three years of data, looking at single electromagnetic showers between 5 and 15 GeV in a model independent way. The 15th International Conference on Flavor Physics & CP Violation 5-9 June, 2017 Prague, Czech Republic * Speaker Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). http://pos.sissa.it/ Searching for LDM in NOvA ND Filip Jediný 1. -
Neutrino Book
The challenge of neutrinos Preparing the Gargamelle bubble chamber at CERN in 1969. In 1973 the chamber took the first historic photographs of neutral current interactions. (Photo CERN 409.9.69) Neutrino book Gargamelle and Neutral Currents - The Story of a Vital Discovery by Andre Rousset Andre Rousset's book (in French - Gargamelle et les Courants Neutres - Ecole des Mines de Paris) tells the story of Gargamelle and the discov ery at CERN in 1973 of neutral currents, the cornerstone of the electroweak theory. This vital discov ery helped to give credence to the Standard Model of particle physics. Rousset is both an observer and one of the key figures in the story. His book is lively and well docu mented; in it he uses archive material to ensure the accuracy of his infor mation on dates, choices and deci sions. ously" to the project was probably in an interesting manner the theo After an introduction to particle what swung the decision. rists' "green light", giving the go- physics which puts into perspective Construction took five years, during ahead to the experimentalists. In fact, the electroweak theory unifying weak which many problems were encoun the European collaboration (Aachen, and electromagnetic interactions, tered, right up to the fault in the main Brussels, CERN, Ecole Polytechni Rousset comes straight to the point. part of the chamber which caused que, Milan, Orsay, UC London) was From the late 1950s onwards he was delays and, a few years later, was to divided between a study of the quark- involved in the construction of the prove fatal to the detector. -
Calibration and Monitoring for the Borexino Solar Neutrino Experiment
Calibration and Monitoring for the Borexino Solar Neutrino Experiment Dissertation submitted to the Faculdade de Ciências da Universidade de Lisboa for the degree of Ph.D. in Physics by José Carvalho Maneira Advisors: Prof. Amélia Maio Prof. Gianpaolo Bellini (University of Milan) Lisbon, November 2001 To my parents and my brother. “The first question I ask myself when something doesn't seem to be beautiful is why do I think it's not beautiful. And very shortly you discover that there is no reason.” John Cage Summary One of the major open issues in Elementary Particle Physics today, the phenomenon of Neutrino Oscillations is a natural consequence of a non-zero neutrino mass and a non-diagonal leptonic mixing matrix. Even if the Standard Model extension to accommodate neutrino oscillations is relatively trivial, a non- zero neutrino mass and mixing is widely considered as a doorway for the Unified Theory of the fundamental interactions. In fact, Super Symmetry naturally explains small neutrino masses through the well-known “see-saw” mechanism. From the experimental point of view, neutrino oscillations are a privileged way of studying the neutrino mass spectrum, since small mass splittings can lead to large and measurable phase differences between interfering quantum-mechanical amplitudes. This is particularly true for Solar Neutrino Experiments, since the large distance between source and detector (1.5´1011 m) allows for a good sensitivity to very small mass differences (down to about 10-11 eV2), not available with the present accelerator and reactor experiments. In fact, the first indication for the possibility of Neutrino Oscillations came from the first measurements of Solar Neutrinos, more than thirty years ago. -
Results of the STEREO Experiment Rudolph Rogly, CEA-Saclay on Behalf of the STEREO Collaboration
Results of the STEREO experiment Rudolph Rogly, CEA-Saclay on behalf of the STEREO collaboration 1 Motivation – Flux anomaly Improved reactor antineutrino spectrum predictions – PRC 83:054615 (2011) Observed ~6.5% deficit in measured fluxes at short-baseline, so- called Reactor Antineutrino Anomaly (RAA) – PRD 83:073006 (2011) ★: RAA oscillation best fit $ $ $ ∆�!"# = 2.3 eV / sin 2�!"# = 0.14 Signature of the oscillation to a sterile state ? 2 Motivation – Shape anomaly Nature Physics 16, 558-564 (2020) ~10% local events excess observed by several lowly enriched in 235U (LEU) experiments around 5 MeV wrt. Huber predicted shape. Related to fuel composition ? Do U and Pu contribute to the same extent ? → Highly-enriched in 235U (HEU) experiments such as STEREO shed a light on the contribution of the pure 235U and are complementary to LEU experiments. 3 The STEREO experiment JINST 13 (2019) 07, P07009 Experimental Site (ILL Grenoble, France): Ø Ground-level experiment. Ø Compact core (∅ 40cm x 80 cm) and short-baseline (~10m) experiment to probe the RAA. 235 Ø 58MWth nominal power / HEU fuel (93% U) → 99% of �̅ flux from 235U fissions. Detector Design: Ø Segmented design for oscillation analysis: 6 cells (target volume) surrounded by 4 gamma catchers. Ø Pb, polyethylene, B4C shielding + water Cherenkov muon veto + Pulse Shape Discrimination for background mitigation and rejection (achieved S:B of 0.8:1). 4 Detector calibration and response PRD 102,052002 (2020) Energy scale derived from a global fit of: q Calibration data taken with point-like radioactive sources in each cell, at different heights. 12 q Cosmogenic B beta spectrum (�! = 13.4 MeV). -
Gigantic Japanese Detector Seeks Supernova Neutrinos Tracing the History of Exploding Stars Is a Goal of the Revamped Super-Kamiokande
NEWS IN FOCUS ASAHI SHIMBUN/GETTY Observations by the Super-Kamiokande neutrino detector have forced theorists to amend the standard model of particle physics. PHYSICS Gigantic Japanese detector seeks supernova neutrinos Tracing the history of exploding stars is a goal of the revamped Super-Kamiokande. BY DAVIDE CASTELVECCHI weight. These data will help astronomers to detector much better at distinguishing between better understand the history of supernovae different types, or ‘flavours’, of neutrino, as well leven thousand giant orange eyes in the Universe — but the neutrinos that the as their antiparticles, antineutrinos. confront the lucky few who have explosions emit have been difficult to detect. In 1987, the Kamiokande detector, Super-K’s entered the Super-Kamiokande under- “Every 2–3 seconds, a supernova goes off smaller predecessor, detected the first neutri- Eground neutrino observatory in Japan — by somewhere in the Universe, and it produces nos from a supernova. The dozen neutrinos far the largest neutrino detector of its kind in 1058 neutrinos,” says Masayuki Nakahata, came from Supernova 1987A, which occurred the world. A chance to see these light sensors who heads the Super-K, an international col- in the Large Magellanic Cloud, a small galaxy is rare because they are usually submerged in laboration led by Japan and the United States. that orbits the Milky Way. Head experimenter 50,000 tonnes of purified water. But a major With the upgrade, the detector should be able Masatoshi Koshiba shared the 2002 Nobel revamp of Super-K that was completed in to count a few of these ‘relic’ neutrinos every physics prize partly for that discovery. -
The Gallex Project Deqq Q05573
BNL-43669 C-3557 BNL—43669 THE GALLEX PROJECT DEQQ Q05573 T.KIRSTEN Max-Planck-Institut für Kernphysik P.OMox 103980 6900 Heidelberg GALLEX GALLEX COLLABORATION: M.Breitenbach, W.Hampel, G.Heusser, J.Kiko, T.Kirsten, H.Lalla, A.Lenzing, E.Pernicka, R.Plaga, B.Povh, C.Schlosser, H.Völk, R,Wink, K.Zuber Max-Planck-Institut für Kernphysik.Heidelberg R.v.Ammon, K.Ebert, E.Henrich, L.Stieglitz Kernforschungszentrum Karlsruhe- KFK ¿Bellota JAN 2 2 Dip.dì Fisica delVUnìversità,Mìlano and Laboratori Nazionali del Gran Sasso-INFN O.Creraonesi, EJFiorini, C.Liguori, S.Ragazzi, L.Zanoiti Dip.di Fisica dell'Università, Milano R.Mössbauer,A.Urban Physik Dept. EIS , Technische Universität München G.Berthomieu, E.Schatzman Université de Nice-Observatoire S.d'Angelo, C.Bacci, P.Belli, R.Bernabei, L.Paoluzi, R.Santonico H-Universita di Roma -INFN M.Cribier, CDupont, B.Pichard, J.Rich, M.Spiro, T.Stolarczyk, C.Tao, D.Vignaud Centre d'Etudes Nucléaires de Saclay, Gif-sur Yvette I.Dostrovsky Weizmann Institute of Sciences,Rehovot G.Friedlander,R.L.Hahn,J.K.Rowley,R.W.Stoenner,J.Weneser Brookhaven National Laboratory, Upton,N.Y. ABSTRACT. The GALLEX collaboration aims at the detection of solar neutrinos in a radiochemical experiment employing 30 tons of Gallium in form of concentrated aqueous Gallium-chloride solution/The detector is primarily sensitive to the otherwise inaccessible pp-neutrinos. Details of the experiment have been repeatedly described before [1-7]. .Here we report the present status of implementation in the Laboratori Nazionali del Gran Sasso (Italy). So far, 12.2 tons of Gallium are at hand.The present status of development allows to start the first full scale run at the time when 30 tons of Gallium become available.This date is expected to be January, 1990. -
Plastic Anti-Neutrino Detector Array (PANDA)
Plastic Anti-Neutrino Detector Array (PANDA) Yo Kato (The University of Tokyo) Yasuhiro KurodaA, Shugo OguriB, Nozomu TomitaA, Ryoko NakataA, Chikara ItoC, Masato TakitaD, Yoshizumi InoueE, Makoto MinowaA,F The University of TokyoA High Energy Accelerator Research Organization (KEK)B Japan Atomic Energy Agency (JAEA)C ICRR, The University of TokyoD ICEPP, The University of TokyoE RESCEU, The University of TokyoF Applied Antineutrino Physics (AAP) Arlington, 7 Dec 2015 Reactor monitoring Inspection by IAEA - Nonproliferation of nuclear technology - Current inspection tools are “intrusive”, such as -- neutron monitoring beside reactor cores -- fuel monitoring before and after reactor operation International Atomic Energy Agency -> Burden for both operator and inspector IAEA proposed a “non-intrusive” inspection tool. Final Report: Focused Workshop on Antineutrino Detection Safeguards Applications (2008) Reactor monitoring using an antineutrino detector - High penetration -> can be detected outside a reactor building - No alternative source -> cannot hide reactor operation -> Suitable for inspection ! 7 Dec 2015 AAP2015 2 Reactor antineutrino Nuclear fission of 235U -> neutron-rich nuclei - 6 antineutrinos - 200MeV per fission decay of neutron-rich nuclei -> antineutrino - - 3GWth reactor emits 6×1020 neutrinos/s Prompt event - Energy deposit of e+ - e+ + e− → 2훾 Delayed coincidence Delayed event gadolinium - Gamma rays by Gd neutron plastic scintillator capture (Total 8 MeV) 7 Dec 2015 AAP2015 3 PANDA(Plastic Anti-Neutrino Detector Array) -
Neutrino Interaction Measurements Using the T2K Near Detectors
Neutrino interaction measurements using the T2K near detectors Daniel G Brook-Roberge for the T2K Collaboration University of British Columbia, Vancouver, BC, Canada E-mail: [email protected] Abstract. The T2K near detectors provide a rich facility for measuring neutrino interactions in a high-flux environment. This talk will discuss the near detector CC-inclusive normalization analysis for the T2K oscillation result in detail, along with the present result, and describe the plan for its extension to more sophisticated measurements. Selection criteria for CCQE interactions will be presented, as will a strategy for calculating cross-section difference between plastic scintillator and water. The unique capacities of the near detectors to measure other exclusive CC and NC channels in a narrow-band off-axis beam will also be explored. 1. Introduction The T2K (Tokai to Kamioka) long-baseline neutrino oscillation experiment[1] aims to make high- precision measurements of oscillation parameters using a beam of muon neutrinos. In particular, the appearance of electron neutrinos in the beam is studied in an effort to measure a non-zero value of the mixing parameter θ13. Electron neutrino appearance provides a particular challenge for the near detector, as the electron neutrino fraction in the muon neutrino beam is the most significant background to this measurement. The T2K experiment has had two experimental runs; one at beam power up to 50 kW from January to June 2010, and one at beam power up to 150 kW from November 2010 to March 2011, when it was cut short by the Tohoku earthquake. 1.43 × 1020 protons on target were accumulated by T2K prior to the earthquake. -
Accurate Measurement of Reactor Neutrinos Close to Surface with STEREO
Accurate measurement of reactor neutrinos close to surface with STEREO Photo:ILL Vladimir Savu IRFU,CEA, Paris-Saclay University on behalf of the STEREO collaboration Vladimir Savu (CEA) 06.12.2019 { AAP 2019 1 / 23 06.12.2019 { AAP 2019 Motivation Sterile neutrino search and reactorν ¯e measurements Motivation of STEREO I Oscillation test L/E ∼ 10 m/3 MeV ! ∼ 1eV sterile neutrino 2 2 Two new parameters: sin (2θnew ) and∆ mnew Physical Review D 83, 073006 (2011), G. Mention et al. 9 ∆ χ 2 4 1 4 9 5.5 Daya Bay Huber model w/ 68% C.L. I absolute flux 5.0 / fission] 4.5 normalization studies 2 cm 43 4.0 − C.L spectral shape studies [10 I 3.5 68% 239 95% σ −43 σ238 =(10.1±1.0)×10 99.7% σ =(6.04±0.60)×10−43 3.0 241 5.2 5.6 6.0 6.4 6.8 7.2 −43 2 σ235 [10 cm / fission] Phys. Rev. Lett. 118, 251801 (2017) Physics Letters B 773 (2017) STEREO will test precisely these 3 questions with a pure 235U spectrum Vladimir Savu (CEA) 06.12.2019 { AAP 2019 1 / 23 The STEREO experiment Experimental site ILL research facility, Grenoble, France Research reactor core 58 MWth ! 1019 ν¯ s−1 e Water channel 15 m.w.e overburden 235 X Highly U enriched X Compact core (40cm ?) X Short baseline measurement: 9.4m < Lcore < 11.2m 93 tons moved on air cushions AutumnAutumn 2016 2016 I Surface-level experiment I γ and neutron background from neighboring experiments Vladimir Savu (CEA) 06.12.2019 { AAP 2019 2 / 23 The STEREO experiment Data taking Data taking I Phase-I: 66 days reactor ON { 22 days reactor OFF I Phase-II: 119 days reactor ON { 211 days reactor OFF I Data