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Atmospheric Neutrino Oscillation

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Atmospheric Neutrino Oscillation Detection of atmospheric neutrino and neutrino oscillation 50Kton ICAL neutrino Detector Shamelessly using slides of Yuichi Oyama (KEK/J-PARC) talk at Vietnam school on Neutrino Historical context Detection of atmospheric neutrinos •Markov (1960) suggests Cherenkov light in deep lake or ocean to detect atmospheric interactions for neutrino physics •Greisen (1960) suggests water Cherenkov detector in deep mine as a neutrino telescope for extraterrestrial neutrinos •First reported events in deep mines with electronic detectors, 1965: KGF detector (Menon et al.), CWI detector (Reines et al.); Two methods for calculating atmospheric neutrinos: •From muons to parent pions infer neutrinos (Markov & Zheleznykh, 1961; Perkins) •From primaries to , K and to neutrinos (Cowsik, 1965 and most later calculations) • Essential features known since 1961: Markov & Zheleznykh, Zatsepin & Kuz’min •Monte Carlo calculations follow second method Stability of matter: search for proton decay, 1980’s backgroundbackground forforpp-decay • IMB & Kamioka -- water Cherenkov detectors • KGF, NUSEX, Frejus, Soudan -- iron tracking calorimeters • Principal background is interactions of atmospheric neutrinos e e • Need to calculate flux of atmospheric neutrinos 0.1 1 10 KGF Cosmic Ray muon experiments 1956 : First experiment by Sreekantan’s group at depth upto 270m But, initiated with simple measurement of muon lifetime experiment in 1949 Geiger counter based telescope measures Cosmic muons intensities at various depth and its angular distributions B V Sreekantan et al Proc Ind Acad Sci 43 (1956) 113 The MNR Experiments, Miyake, Narasimham and Ramanamurthy 1961 : New Series of Cosmic muon Experiments started by TIFR in KGF depths from 270m to 2760m The MNR group measure flux around 6 different depths and found at 2760m muon flux is attenuated This led to the observation neutrino at deep underground S Miyake, V S Narasimham, P V Ramana Murthy Nuovo Cim 32 (1964) 1505; 32 (1964) 1524 First report on Atmospheric neutrinos Atmospheric neutrino detector at Kolar Gold Field –1965 Physics Letters 18, (1965) 196, dated 15th Aug 1965 PRL 15,PRL (1965), 15, 429,(1965), dated 429, 30th dated Aug. 30th 1965 Aug. 1965 KGF muon and neutrino experiments Collaboration: INDIA , UK and Japan Inelastic collision of an upward-moving neutrino Neon Flash Tubes Observed neutrino induced muon events predicted MW > 3 GeV 2.5 Lead Anomalous Kolar events : Event consists of two or more tracks and vertex of tracks pointing in air/low mass mat ! S Miyake, V S Narasimham, P V Ramana Murthy Nuovo Cim 32 (1964) 1505; ibid 32 (1963) 1524 KGF neutrino and proton decay experiments Collaboration: INDIA , UK and Japan Proton Decay Experiment 140 ton (at 2.3 km) Absorber : Iron ½” Detector : 10cm 10cm 4(6)m Proportional counter 8.41years Prof. NK Mondal’s thesis 5.53years 340 ton (at 2km) 60 horizontal array V = 6m 6m 6m Underground lab The rate of the atmospheric neutrino interactions is about 200 kt−1 year−1. Rate at the surface due to cosmic ray particles is very frequent, namely ∼200 m−2 s−1, Deepest experimental halls : EPR Mine in South Africa : ) 8800 m.w.e KGF : Deepest : 8400m.w.e (whereas neutrino discovery INO at 7500m.w.e neutrino+proton KGF ( KGF KGF (cosmic KGF muon flux) EPR Mine, South AFRICA South Mine, EPR History of Discoveries by neutrino experiments 1956 Reines and Cowan discovered anti-electron neutrino from a reactor (N) 1962 Muon neutrino beam experiment by L.Lederman et al (N) 1965 KGF observed atmospheric neutrino 1968 Homestake experiment claimed solar neutrino deficit (N) 1973 Neutral Current interaction was discovered by Gargamelle 1987 Kamiokande and IMB detected neutrinos from supernova SN1987A (N) Starting point of neutrino astronomy 1988 Kamiokande claimed atmospheric muon neutrino deficit 1989 Kamiokande confirmed the solar neutrino deficit 1998 Super-Kamiokande observed atmospheric neutrino oscillation (N) 1998 Super-Kamiokande confirmed solar neutrino deficit 2000 DONUT observed tau neutrino 2001 SNO confirmed solar neutrino oscillation by neutral current measurement (N) 2002 Kamland observed deficit of reactor neutrinos 2004 K2K confirmed atmospheric neutrino oscillation by artificial neutrino beam 2006 Completely independent confirmation of -t oscillation by MINOS 2012 Non-zero q13 was confirmed by 3 reactor experiments 2015 Discovery of t signal from - t oscillation by OPERA Solar neutrino oscillation? Homestake experiment claimed solar neutrinos deficit for over 15 years until middle of 1980s. However, not many people consider the result seriously. SSM calculation Total neutrino flux seems to be certainly robust. It can be directly evaluated from the solar luminosity. However, Homestake experiment does not measure pp neutrino. Other neutrino components are small fractions and not robust. It strongly depend on core temperature, chemical composition, cross sections, opacity of the Sun, etc. We cannot believe the calculation ! Homestake experiment Experiments in ~1MeV energy range are not territory of high energy physicists. R. Davis was not a physicist, but a chemist. Radiochemical method is not common technology for high energy physicists. Most of our experiments are "counter experiments". We cannot imagine/understood the experiment ! No experiment followed Homestake. (1 SNU is 10-36 captures per target atom per second) Atmospheric neutrinos p,He,… Primary cosmic rays (p, He,…) collide with upper atmosphere and neutrinos are produced. ± + e + e + e e : ~ 1 : 2 Particles and anti-particles are not distinguished unless needed. + For example, + means 흅 → + − − 흁 + 흂흁 풂풏풅 흅 → 흁 + 흂ഥ흁 in most of the e experiment except INO-ICAL Kamiokande (1983-1996) A large water Cherenkov detector constructed at 1000 m (2400 meter water equivalent) underground in Kamioka mine, Japan. 3000 tons of pure water are viewed by 1000 20-inchF PMTs. In KAM-I, the trigger threshold of the detector was ~29 MeV, was enough to detect nucleon decay mode pK+(+) Fall 1984 to end of 1986, detector upgraded to observe 8B solar neutrinos • KAM-I: trigger threshold of 110 photoelectrons (p.e.), which corresponds to 30 MeV/c (at 50% efficiency) and 37 MeV/c (90%) for electrons (3.4 p.e.=1 MeV for electrons), and 205 MeV/c (50%) and 220 MeV/c (90%) for muons. • KAM-II : 7.6 MeV/c (50%) and 10 MeV/c (90%) for electrons, and 165 MeV/c (50%) and 180 MeV/c (90%) for muons e/ identification in Kamiokande e e Cherenkov light from electromagnetic shower. Electrons and positrons are heavily scattered. Cherenkov ring edge is fuzzy. e e Only direct Cherenkov light from Clear Cherenkov ring edge Simulation : ± ± 흅 → 흁 ퟓ. ퟒ ± ퟎ. ퟖ % 흅ퟎ → 풆± ퟔ. ퟕ ± ퟏ. ퟐ % e/ misidentification probability is less than 1 %. “Experimental study of the atmospheric neutrino flux” The first Kamiokande paper on atm neutrino : Phys. Lett B205 (1988) 416 2.87 kt*yr data e data 93 data 85 data MC MC 88.5 MC 144.0 Single ring e-like 93 88.5 Single ring -like 85 144.0 Multi ring 87 86.2 total 265 318.7 e-like : good agreement -like : data/MC = 59±7% (stat) e data 93 data 85 Were unable to explain the data as the MC 88.5 MC 144.0 result of systematic detector effects or uncertainties in the atmospheric neutrino fluxes. Some as-yet-unaccounted-for physics such as neutrino oscillations might explain the data. “Observation of a Small /e Ratio in Kamiokande” The second Kamiokande paper on atm neutrino : Phys. Lett B280 (1992) 146 4.92 kt*yr data, 310 single ring events data MC1 MC2 MC3 e data 159 1992論文 MC1 164.9 Single ring e-like 159 164.9 146.0 127.7 MC2 146.0 MC3 127.7 Single ring -like 151 260.6 234.2 205.2 data 151 MC1151 260.6 MC2260.6 234.2 MC3234.2 205.2 205.2 data/e data expected/e expected Observation of a Small /e …… (continued) "Neutrino Oscillation" was discussed positively. sin22q-Dm2 plot was officially reported first time. Absolute atmospheric neutrino flux is ambiguous but /e ratio is robust. -t oscillation is favored, but -e cannot be denied, but ruled out by solar neutrino result. Other experimental curves are exclusion plot -e -t -t Best fit (sin22q,Dm2)= (0.87,0.8 10-2eV2) e t -e Best fit in 2016 (sin22q,Dm2)= e t (1.00,2.5110- 2eV2) NUSEX experiment (1982-1988) The NUSEX detector is a digital tracking calorimeter of 3.5m 3.5m 3.5m, located in Mont Blanc tunnel at 4800 m.w.e. underground. It is a sandwich of 134 horizontal iron plates of 1.0 cm thickness, and layers of plastic streamer tubes 3.5 m long and of (9 9) mm2 cross-section. The total active mass is 150 ton. From 740 ton * yr of exposure, data agree with Monte Carlo expectation. data 32 e data 18 expected 36.8 expected 20.5 R=(data/MC)/(edata/eMC) +0.32 =0.96 -0.28 Europhys. Lett. 8 (7) (1989) 611 Frejus experiment (1984-1988) The Frejus detector is located in the Frejus highway tunnel connecting France and Italy. ｄata 108 The rock coverage is 1780m. expected 125.8 It consists of 912 flash chamber planes and 113 1.56kton・yr data Geiger tube planes. A flash chamber plane is made of a sandwich of 3 mm thick iron plates and 5 mm thick plane of plastic flash tubes (discharge on Ne-He filled chamber). The fiducial mass is 554 tons. Good agreement is obtained between the data and the simulation within statistics. e Data 57 expected 70.6 Phys. Lett B227 (1989) 489 IMB-3 experiment Data from 851 days of IMB-3 experiment are analyzed. A total of 935 contained atmospheric neutrino events areaccumulated from 7.7 kton・yr of exposure. PhysRev D46 (1992) 3720 data Monte Carlo Nonshower Nonshowering 182 268.0 300 < p < 1500 MeV ( -like single ring) data 182 MC 268.0 Showering 〇: all data 352 257.3 ×: ->e signal (e-like single ring) The fraction of nonshowering events is Data: 0.36±0.02(stat)±0.
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