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

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xyEvent: 470, Entry: 470, Time Tue Aug 31 17:32:33 2010nhit0: 96, nhit1: 95Figure E.1: A typical noise event where all tubes show a signal. The colors indicatethe signal width: pink for medium and turquoise for small widths.xyEvent: 4758, Entry: 4758, Time Thu Sep 2 21:36:23 2010nhit0: 7, nhit1: 5Figure E.2: A typical noise event of RUN 243 11-23-20 where tubes on the rightshow a signal. The colors indicate the signal width: pink for medium and turquoisefor small widths.110
Bibliography[1] W. Pauli. Dear radioactive ladies and gentlemen. Phys. Today, 31N9:27, 1978.[2] Frederick Reines and Clyde L. Cowan. The neutrino. Nature, 178:446–449,1956.[3] G. Danby et al. Observation of High-Energy Neutrino Reactions and the Existenceof Two Kinds of Neutrinos. Phys. Rev. Lett., 9:36–44, 1962.[4] Martin L. Perl. The New Particles Produced in electron-Positron Annihilation.Presented at Symposium on New Directions in Hadron Spectroscopy, ArgonneNational Lab., Ill., Jul 7-10, 1975.[5] R. Rameika. The DONUT experiment: First direct evidence of nu/tau. Preparedfor 28th SLAC Summer Institute on Particle Physics: Neutrinos fromthe Lab, the Sun, and the Cosmos (SSI 2000), Stanford, California, 14-25 Aug2000.[6] Precision electroweak measurements on the Z resonance. Phys. Rept., 427:257,arXiv:hep-ex/0509008.[7] Raymond Davis, Jr., Don S. Harmer, and Kenneth C. Hoffman. Search forneutrinos from the sun. Phys. Rev. Lett., 20:1205–1209, 1968.[8] P. Anselmann et al. Solar neutrinos observed by GALLEX at Gran Sasso. Phys.Lett., B285:376–389, 1992.[9] M. Altmann et al. Complete results for five years of GNO solar neutrino observations.Phys. Lett., B616:174–190, arXiv:hep-ex/0504037.[10] A. I. Abazov et al. Search for neutrinos from sun using the reaction Ga-71(electron-neutrino e-) Ge-71. Phys. Rev. Lett., 67:3332–3335, 1991.[11] K. S. Hirata et al. Observation of B-8 Solar Neutrinos in the Kamiokande-IIDetector. Phys. Rev. Lett., 63:16, 1989.[12] Y. Fukuda et al. Evidence for oscillation of atmospheric neutrinos. Phys. Rev.Lett., 81:1562–1567, arXiv:hep-ex/9807003.[13] Q. R. Ahmad et al. Measurement of the charged current interactions producedby B-8 solar neutrinos at the Sudbury Neutrino Observatory. Phys. Rev. Lett.,87:071301, arXiv:nucl-ex/0106015.111
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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
Page 68 and 69: (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
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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 120 and 121: [14] Ch. Kraus et al. Final Results
Page 122 and 123: [49] T. Araki et al. Experimental i
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Page 126: Jan Lenkeit und Björn Wonsak sowie
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