Etude et impact du bruit de fond corrÃ©lÃ© pour la mesure de l'angle ...

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24 2. Neutrino physics tel-00821629, version 1 - 11 May 2013 detector is approximately independent from the distance L (the oscillation goes ⇠ (L/E) 2 and the neutrino flux diminish as 1/L 2 ). In the opposite limit where 1 the oscillation are so fast that get averaged out, P (⌫ ↵ ! ⌫ ) ' 1/2sin 2 2✓. In this limit the oscillation probability does not depend from the oscillation phase and the number of oscillation events decrease as 1/L 2 . In order to measure both oscillation parameters, the measurement of the averaged probability is not enough, moreover the L (or E) dependence must also be measured to characterise the oscillation pattern. The best possible experimental condition to characterise oscillation parameters is then to have an oscillation phase of ' 1. Even if three neutrino families exist, the mixing parameters are such that the dominant oscillation pattern is driven by the two flavour mixing, while the third flavour contribute at the second or higher order. For this reason the results of oscillation experiments are often shown in a two neutrino scenario and determine a single mixing angle and squared mass di↵erence. 2.4.1 Experimental determination of m 2 12 and ✓ 12 Measurement of m 2 12 and ✓ 12 oscillation parameters has been performed by Super-Kamiokande (SK) and SNO using neutrino created in the thermonuclear reaction produced in the sun. The same parameters has also been measured by KamLAND using terrestrial ¯⌫ e emitted by nuclear power plant. Results from global analysis is shown in Fig. 2.2 [91]. Solar neutrinos Solar neutrino are ⌫ e coming from the process responsible for solar power production: 4p +2e ! 4 He +2⌫ e + 26.7 MeV. The process take place through di↵erent reactions and consequently solar neutrino are characterised by di↵erent energy spectra as shown in Fig. 2.3 [39]. The typical neutrino flux reaching the earth is of about 10 8 ⌫/s/m 2 . Several experiments measured the solar neutrino flux, starting with the pioneering Chlorine experiment in the Homestake mine, proposed by Davis [50]. The ⌫ e flux were measured in a tank of 400 m 3 of C 2 Cl4 counting the number of radioactive Ar nuclei produced by the inverse beta decay reaction 37 Cl + ⌫ e ! Ar + e . Only one third of the neutrino flux predicted by the Standard Solar Model were measured. At that time an error on the experimental measurements or in the Standard Solar Model was assumed as possible explanation of the observed deficit. While error in the theoretical model were excluded by a better understanding of the sun, further experimental measurements, performed with di↵erent technique by Gallex [61], Sage/GNO [13] and Super Kamiokande [63] confirmed the deficit in the solar neutrino flux.
3-flavour oscillations The dominanting oscillation modes 2.4 Measuring neutrino oscillation parameters 25 4 "m 2 21 [ 10-5 eV 2 ] 15 10 5 solar neutrino exps. combined ! KamLAND ∆m 2 31 [ 10-3 eV 2 ] 3 2 MINOS tel-00821629, version 1 - 11 May 2013 0 0.2 0.4 0.6 0.8 sin 2 ! 12 Figure 2.2: m 2 12 and ✓ 12 parameters from global analysis of solar and reactor experiments [91]. 1 0 0.25 sin 2 ✓ 12 0.3 sin 2 ✓ 23 0 m21 2 m31 2 1 30 T. Schwetz Di↵erent processes contributing to the solar neutrino spec- Figure 2.3: trum [39].
Page 1 and 2: UNIVERSITÉ DENANTES FACULTÉ DES S
Page 3 and 4: tel-00821629, version 1 - 11 May 20
Page 5 and 6: Abstract tel-00821629, version 1 -
Page 7 and 8: Acknowledgments Since so many peopl
Page 9 and 10: Contents 1 Introduction 13 tel-0082
Page 11 and 12: CONTENTS 11 tel-00821629, version 1
Page 13 and 14: Chapter 1 Introduction tel-00821629
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Page 17 and 18: Chapter 2 Neutrino physics tel-0082
Page 19 and 20: 2.2 Neutrino history in brief 19 ma
Page 21 and 22: 2.3 Neutrino oscillation, the theor
Page 23: 2.4 Measuring neutrino oscillation
Page 27 and 28: 2.4 Measuring neutrino oscillation
Page 29 and 30: After the Sun, the other main natur
Page 35 and 36: 2.5 The problem with the neutrino m
Page 37 and 38: 2.6 Summary and open questions 37 s
Page 39 and 40: In the next future, reactor experim
Page 41 and 42: Chapter 3 The Double Chooz experime
Page 43 and 44: 3.1 The Double Chooz detector 43 to
Page 45 and 46: 3.1 The Double Chooz detector 45 te
Page 47 and 48: 3.1 The Double Chooz detector 47 it
Page 49 and 50: 3.1 The Double Chooz detector 49 te
Page 51 and 52: 3.2 The detector read-out 51 40 m o
Page 53 and 54: 3.3 The online system 53 IV trigger
Page 55 and 56: 3.3 The online system 55 tions as s
Page 57 and 58: 3.3 The online system 57 tel-008216
Page 59 and 60: 3.4 The calibration system 59 tel-0
Page 61 and 62: loosing their kinetic energy 3 and
Page 63 and 64: 3.5 Reactor neutrino flux simulatio
Page 69 and 70: 3.8 Data reconstruction 69 A dedica
Page 71 and 72: Regarding the pulse information, th
Page 73 and 74: 3.8 Data reconstruction 73 tel-0082
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3.8 Data reconstruction 75 Gain (ch
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3.9 Conclusions 77 tel-00821629, ve
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Chapter 4 Measurement of ✓ 13 wit
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4.1 Data sample 81 create a signal
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4.2 ¯⌫ e signal selection 83 Liv
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4.2 ¯⌫ e signal selection 85 Pro
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4.2 ¯⌫ e signal selection 87 Neu
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4.3 Backgrounds 89 energy spectrum
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4.3 Backgrounds 91 tel-00821629, ve
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4.4 Selection e ciencies and system
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4.4 Selection ! e ciencies and syst
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4.5 Data analysis summary 99 4.4.3
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4.6 Final fit and measurement of
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4.6 Final fit and measurement of
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4.7 Summary and Conclusions 105 tel
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Chapter 5 Correlated background tel
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5.1 Measuring correlated background
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5.2 High energy analysis 111 in a l
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5.2 High energy analysis 113 tel-00
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5.3 OV Tag analysis 115 The t cut v
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5.4 Fast Neutrons analysis 117 bigg
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5.4 Fast Neutrons analysis 119 5.4.
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5.4 Fast Neutrons analysis 121 tel-
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5.4 Fast Neutrons analysis 123 esti
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5.4 Fast Neutrons analysis 125 Corr
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5.4 Fast Neutrons analysis 129 Prom
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5.4 Fast Neutrons analysis 131 lect
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5.4 Fast Neutrons analysis 133 mari
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5.5 Stopping Muon analysis 139 5.5.
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5.5 Stopping Muon analysis 141 tel-
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5.5 Stopping Muon analysis 143 tel-
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5.5 Stopping Muon analysis 145 Sour
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5.5 Stopping Muon analysis 147 belo
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5.5 Stopping Muon analysis 149 The
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5.6 Estimation of correlated backgr
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5.7 Conclusion 157 5.7 Conclusion t
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Chapter 6 Conclusions tel-00821629,
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161 • The SM analysis could be im
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Chapter 7 Contributions to Double C
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165 from this study and from [64] f
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List of Figures tel-00821629, versi
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LIST OF FIGURES 169 tel-00821629, v
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List of Tables 3.1 Mean energy rele
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Bibliography [1] [2] tel-00821629,
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BIBLIOGRAPHY 183 [31] J.K. Ahn et a
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BIBLIOGRAPHY 185 [61] W. Hampel et
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BIBLIOGRAPHY 187 [92] A. Stueken et
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