Setup of a Drift Tube Muon Tracker and Calibration of Muon ...

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[14] Ch. Kraus et al. Final Results from phase II of the Mainz Neutrino Mass Searchin Tritium β Decay. Eur. Phys. J., C40:447–468, arXiv:hep-ex/0412056.[15] V. M. Lobashev et al. Direct search for neutrino mass and anomaly in thetritium beta-spectrum: Status of ’Troitsk neutrino mass’ experiment. Nucl.Phys. Proc. Suppl., 91:280–286, 2001.[16] A. Osipowicz et al. KATRIN: A next generation tritium beta decay experimentwith sub-eV sensitivity for the electron neutrino mass. arXiv:hep-ex/0109033.[17] Ettore Majorana. Theory of the Symmetry of Electrons and Positrons. NuovoCim., 14:171–184, 1937.[18] Stefan. Schönert et al. The GERmanium Detector Array (GERDA) for thesearch of neutrinoless beta beta decays of Ge-76 at LNGS. Nucl. Phys. Proc.Suppl., 145:242–245, 2005.[19] C. Arnaboldi et al. CUORE: A cryogenic underground observatory for rareevents. Nucl. Instrum. Meth., A518:775–798, arXiv:hep-ex/0212053.[20] R. Arnold et al. Technical design and performance of the NEMO 3 detector.Nucl. Instrum. Meth., A536:79–122, arXiv:physics/0402115.[21] B. Pontecorvo. Mesonium and antimesonium. Sov. Phys. JETP, 6:429, 1957.[22] B. Pontecorvo. Neutrino experiments and the question of leptonic-charge conservation.Sov. Phys. JETP, 26:984–988, 1968.[23] Ziro Maki, Masami Nakagawa, and Shoichi Sakata. Remarks on the unifiedmodel of elementary particles. Prog. Theor. Phys., 28:870–880, 1962.[24] Y. Ashie et al. A Measurement of Atmospheric Neutrino Oscillation Parametersby Super-Kamiokande I. Phys. Rev., D71:112005, arXiv:hep-ex/0501064.[25] P. Adamson et al. Measurement of Neutrino Oscillations with the MINOSDetectors in the NuMI Beam. Phys. Rev. Lett., 101:131802, arXiv:0806.2237.[26] M. Ambrosio et al. Measurements of atmospheric muon neutrino oscillations,global analysis of the data collected with MACRO detector. Eur. Phys. J.,C36:323–339, 2004.[27] M. H. Ahn et al. Measurement of Neutrino Oscillation by the K2K Experiment.Phys. Rev., D74:072003, arXiv:hep-ex/0606032.[28] J. Hosaka et al. Three flavor neutrino oscillation analysis of atmospheric neutrinosin Super-Kamiokande. Phys. Rev., D74:032002, arXiv:hep-ex/0604011.[29] B. Aharmim et al. Low Energy Threshold Analysis of the Phase I and PhaseII Data Sets of the Sudbury Neutrino Observatory. Phys. Rev., C81:055504,arXiv:0910.2984.[30] S. Abe et al. Precision Measurement of Neutrino Oscillation Parameters withKamLAND. Phys. Rev. Lett., 100:221803, arXiv:0801.4589.112
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Setup of a Drift Tube Muon Trackera
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AbstractIn this work the setup and
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3.5.5 Pattern Recognition . . . . .
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viii
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essential for vetoing these events.
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Chapter 2NeutrinosThe standard mode
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However, it did not yet deliver an
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Table 2.1: Neutrino oscillation par
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this assumption, the Standard Solar
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Figure 2.1: Neutrino flux at Earth
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asymmetry between neutrino and anti
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Figure 2.3: Expected ¯ν e energy
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Nb neutrino/fission-11010-2Neutrino
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108−dE/dx (MeV g −1 cm 2 )65432
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Figure 3.3: Setup of the muon track
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zyxModule b.0Module a.0Module b.1Mo
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Figure 3.6: Display of the slow con
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plastic scintillators. To avoid all
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N hitsHitmap Plane 06000h_hitmap0En
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Table 3.4: Data structure for calib
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TDC SpectrumN/[2 Channels]1000800H_
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Table 3.5: List of variables calcul
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with ∆⃗q = ⃗q n − ⃗q n−
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N [a.u.]∆ α (x)2200020000da0Entr
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d[mm]Reco Drift Distances201816H_RE
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N [a.u.]Real DataReal data0.06MCh1E
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χ 2N [a.u.]Probability103×10hc2p0
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N [a.u]Residuals20001800h0Entries 3
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Counts/(10 keV × day × 100 tons)1
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4.1.3 Čerenkov LightČerenkov dete
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4.2 The Borexino DetectorThe Borexi
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muons, is reduced by going deep und
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(typically below 50 cm), the locati
Page 70 and 71: 510Counts/(10 keV x day x 100 tons)
Page 72 and 73: counts/days*4 hitsDay (Red) and Nig
Page 74 and 75: eeSurvival probability for ν e, P0
Page 76 and 77: the CMT to the Borexino tracking, t
Page 78 and 79: P C P DSCINT C SCINT DySCINT BSCINT
Page 80 and 81: Figure 5.2: The CMT setup on top of
Page 82 and 83: Angular AcceptanceAngular Acceptanc
Page 84 and 85: Comparison nhits=3 vs nhits=4N [a.u
Page 86 and 87: Table 5.3: Overview of all muon run
Page 88 and 89: N/dayAll Triggers vs Time12000h_tim
Page 90 and 91: Reco Hits in Scintillatory [mm]1000
Page 92 and 93: PMTPMTScintillatorPMTPMTFigure 5.16
Page 94 and 95: the CMT data file and the Borexino
Page 96 and 97: Zenith Angle CMT and BX-GL Tracks h
Page 98 and 99: Lateral x Resolution CMT - IDhlatx_
Page 100 and 101: Distance d between CMT and BX-GL Tr
Page 102 and 103: Angular difference αN [arbitrary u
Page 104 and 105: [m]z bxTrack Position in BX x=0 Pla
Page 106 and 107: N [arbitrary units]∆y all data200
Page 108 and 109: To determine the Borexino tracking
Page 110 and 111: Table A.1: Variables that can be se
Page 112 and 113: espectively. The channel numbers ar
Page 114 and 115: xyϕϕ ′βx ′µFigure C.2: Rela
Page 116 and 117: the z-coordinate z op,0 of the firs
Page 118 and 119: xyEvent: 470, Entry: 470, Time Tue
Page 122 and 123: [49] T. Araki et al. Experimental i
Page 124 and 125: 116
Page 126: Jan Lenkeit und Björn Wonsak sowie
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