Analysis of Neutrino Oscillation experiments
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1 Analysis of Neutrino Oscillation experiments Mario Andrés Acero Ortega Università degli Studi di Torino, LAPTH - Université de Savoie Second Year - Seminar Torino, Italy January 15th, 2008 Tutor: Carlo Giunti (INFN - Torino) Co-Tutor: Julien Lesgourgues (LAPTH - Annecy) Analysis of Neutrino Oscillation experiments p. 1
2 1. Outline Neutrino oscillations Analysis of Neutrino Experimental Data Gallium experiments Reactor experiments Conclusions What is coming... Analysis of Neutrino Oscillation experiments p. 2
3 2. Neutrinos oscillations Quantum mechanical phenomenon interference of different massive νs. Oscillations between active neutrino flavors they are massive and mixed. We can detect νs through Charged- or neutral current processes (ν e + 71 Ga 71 Ge + e used in gallium experiments); Elastic scattering ν + e ν + e. Analysis of Neutrino Oscillation experiments p. 3
4 3. Analysis of Neutrino Experimental Data Experimental evidence of three-neutrino mixing from solar and atmospheric neutrino experiments: m 2 sol = ( ) 10 5 ev 2 m 2 atm ev 2 But... Anomalies which can be interpreted as exotic neutrino mixing: LSND (but with MiniBOONE...), Gallium radioactive source experiments GALLEX, SAGE. Possible explanation: disappearance of electron neutrinos due to neutrino oscillation (ν e ν s ). Then we analyze the Gallium experiment data and study the compatibility with the data from Bugey and CHOOZ reactor experiments Two Neutrino Mixing framework. Analysis of Neutrino Oscillation experiments p. 4
5 3.1 Ga experiments: GALLEX and SAGE Electron neutrinos come from the decay of 51 Cr and 37 Ar radioactive sources which decay through electron capture emiting monoenergetic ν e detected through the reaction Solar Seutrino Experiments ν e + 71 Ga 71 Ge + e. 1.1 GALLEX Cr1 SAGE Cr p(measured)/p(predicted) GALLEX Cr2 SAGE Ar Weighted average R = 0.88 ± Analysis of Neutrino Oscillation experiments p. 5
6 3.2 Ga experiments The survival probability of electron (anti)neutrinos with energy E at a distance L from the source is ( P νe ν e (L, E) = 1 sin 2 (2θ) sin m2 (ev 2 ) )L(m), E(MeV ) Electron capture Cr + e V + ν e For the analysis we use the theoretical ratio, R th, of the predicted 71 Ge production rates with and without neutrino oscillations: R th = dv L 2 i B iσ i P νe ν e (L, E i ) i B, iσ i dv L 2 37Ar (35.04 days) which is to be compared with the measured ratios. 37Cl (stable) 813 kev ν ( 9.8%) 811 kev ν (90.2%) Analysis of Neutrino Oscillation experiments p. 6
7 3.3 Ga experiments σ allowed bands for GALLEX-Cr2 and SAGE 37 Ar, with m 2 1eV 2. m 2 [ev 2 ] m 2 [ev 2 ] Gallex Cr1 Gallex Cr % C.L. (1σ) 68.27% C.L. (1σ) 95.45% C.L. (2σ) 95.45% C.L. (2σ) 99.73% C.L. (3σ) 99.73% C.L. (3σ) sin 2 2ϑ SAGE 51 Cr SAGE 37 Ar 68.27% C.L. (1σ) 68.27% C.L. (1σ) 95.45% C.L. (2σ) 95.45% C.L. (2σ) 99.73% C.L. (3σ) 99.73% C.L. (3σ) 10 2 m 2 [ev 2 ] m 2 [ev 2 ] sin 2 2ϑ sin 2 2ϑ sin 2 2ϑ Analysis of Neutrino Oscillation experiments p. 7
8 3.4 Ga experiments 10 8 Combined least-squares analysis for the Gallium experiments. It shows a 1σ allowed region, and we find χ Gallium 99.73% C.L % C.L % C.L. m 2 bf = 2.03eV sin 2 (2θ) bf = and at 1σ (68.27 % C.L.) m 2 > 0.84eV 2 sin 2 (2θ) bf = m ν 2 (ev 2 ) sin 2 (2θ) χ 2 Analysis of Neutrino Oscillation experiments p. 8
9 4. Reactor experiments Electron antineutrino detected through the inverse beta decay process ν e + p n + e + with the energy relation E ν = E e MeV. The Bugey experiment searches for ν e disappearance at the three distances (L j = 15, 40, 95 m) and collected N j = 25, 25, 10 (for j = 1, 2, 3) energy bins (data). Analysis of Neutrino Oscillation experiments p. 9
10 4.1 Bugey Narrow 1σ allowed region with m 2 arround 1.85eV 2 and 0.02 sin 2 2θ 0.08 χ Bugey 68.27% C.L. (1σ) 95.45% C.L. (2σ) 99.73% C.L. (3σ) 10 m 2 [ev 2 ] sin 2 2ϑ χ 2 Analysis of Neutrino Oscillation experiments p. 10
11 4.2 Bugey spectra Histogram relative to the best fit against the Bugey experimental data sin 2 2θ bf = m 2 bf = 1.85eV2 R R E e + [MeV] E e + [MeV] R E e + [MeV] Analysis of Neutrino Oscillation experiments p. 11
12 4.3 Chooz Chooz B Nuclear Power Station 2 x 4200 MWth The ratio of the number of observed to the expected events (in absence of oscillations) is R Chooz = 1.01 ± P νe ν e (L, E) = 1 sin 2 (2θ)sin m2 (ev 2 «)L(m) average to E(MeV ) distance = 1.0 km neutrino target ν Depth 300 mwe P νe ν e = sin2 2θ, Chooz Underground Neutrino Laboratory Ardennes, France Experiment L E m 2 Bugey (SBL) 10 m 1 MeV 0.1 ev 2 Chooz (LBL) 1 km 1 MeV 10 3 ev 2 Which is then combined with the previous analysis, in the m 2 scale we are interested in ( m 2 1 ev 2 ). Analysis of Neutrino Oscillation experiments p. 12
13 4.3 Global fit Weak indication in favor of neutrino oscillations with and m eV sin 2 2θ m 2 [ev 2 ] χ Ga + Bugey + Chooz 68.27% C.L. (1σ) 95.45% C.L. (2σ) 99.73% C.L. (3σ) sin 2 2ϑ χ 2 Analysis of Neutrino Oscillation experiments p. 13
14 6. Conclusions From Gallium experiments, we found and indication of neutrnio disappearance due to neutrino oscillations with sin 2 2θ 0.04 and m ev 2. The Bugey data present a weak indication in favor of neutrino oscillations with 0.02 sin 2 2θ 0.08 and m ev 2. In the combined analysis of the Gallium, Bugey and CHOOZ data, the weak indication persists, with compatible results between the Bugey-Gallium, Bugey-CHOOZ and Gallium-CHOOZ data analysis. Work published: M.A., C. Giunti, M. Laveder, Limits on ν e and ν e disappearance from Gallium and reactor experiments, arxiv: Analysis of Neutrino Oscillation experiments p. 14
15 Future work Extending the data analysis including some other reactor experiments, which show anomalies that could be indication of neutrino oscillations. CHOOZ (complete analysis) Savannah River Site Institute Laue Langevin (I.L.L) Gösgen Studying constrains in sterile neutrinos, coming from cosmological data (work under the supervision of Julien Lesgourgues and Carlo Giunti) Thanks! Analysis of Neutrino Oscillation experiments p. 15
16 Back Analysis of Neutrino Oscillation experiments p. 16
Carlo Giunti. CERN Particle and Astro-Particle Physics Seminar. work in collaboration with Mario Acero Marco Laveder Walter Winter
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