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

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espectively. The channel numbers are values between 1 and 96 in the binary data.During data read out they are decreased by 1, so that the resulting channel numbergo from 0 to 95. The last channel sequence is followed by0x 4400 0000indicating the end of the event. This is followed either by the next event or a newcycle.104
Appendix CCMT Setup at Gran SassoIn the Appendix, some schematic drawings for the better understanding of the currentCMT setup are presented. Fig. fig:bxcmtmap depicts the channel mapping ofthe CMT. In Fig. C.2, the rotation of the CMT reference system with respect to theBorexino system is presented.TDC 111109876543210595857565554535251504948232221201918171615141312717069686766656463626160353433323130292827262524838281807978777675747372474645444342414039383736959493929190898887868584TDC 011109876543210595857565554535251504948232221201918171615141312717069686766656463626160353433323130292827262524838281807978777675747372474645444342414039383736959493929190898887868584Figure C.1: Channel map for each tube for the current CMT setup.105
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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
Page 62 and 63: 4.1.3 Čerenkov LightČerenkov dete
Page 64 and 65: 4.2 The Borexino DetectorThe Borexi
Page 66 and 67: 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
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 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 120 and 121: [14] Ch. Kraus et al. Final Results
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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