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

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PMTPMTScintillatorPMTPMTFigure 5.16: Trigger layout after the foreseen trigger update (not to scale).xyα0: 6.018417, α1: 5.923773, θ: 0.433896, ϕ: 4.087303nhit0: 3/12, nhit1: 4/8Event: 960, Entry: 177, Time: Mon May 24 01:54:24 2010Figure 5.17: A multiple muon event in the CMT. Due to the setup of the detector,a distinct 3D reconstruction is not possible and the event has to be rejected.84
N/dayTime Distribution of BX CMT Flagged events (3 ≤nhit ≤12)98htimeeventEntries 582Mean 1.273e+09RMS 5.483e+067654321031/01 02/03 01/04 01/05 31/05 30/06 30/07 29/08DateFigure 5.18: Time distribution of common events in Borexino and the CMT. Atriggered signal is considered an event, if three or more, but no more than twelve tubeshave been hit in each plane. The gaps in the distribution come from periods wherethe CMT did not take data.5.3 Common Events with BorexinoDespite the poor trigger efficiency of roughly 50%, some tracks passing both theCMT and Borexino could be reconstructed.Due to the trigger setup, events are also recorded when the track does not crossthe CMT detector or passes only an insufficient number of tubes. To get a firstestimate of which occurrences can be considered true events, the basic following cutis applied: In each 2D plane, at least three hits have to be recorded. Also, themaximum number of hits must not exceed twelve. The latter cut is mainly used toreduce noise events from the data. Fig. 5.18 shows the distribution of coincidenceevents over time. It can easily be seen that due to the malfunctioning trigger thedaily number of events is well below the expected value of ∼ 9.6 events per dayfrom the simulation. Altogether, there are 582 events qualifying for reconstruction.However, the basic event selection based on the number of hits also includes certainnoise patterns so that in the end only 392 events could be reconstructed. Usingthese events, a first analysis of the Borexino muon tracking was performed.5.3.1 Borexino Data MatchingBorexino and CMT data are matched on an event by event basis using the timestampof each event. As mentioned before, the CMT trigger signal is also sent to theBorexino DAQ, where a flag is set in case of a common event. From the Borexinodata, all events with a CMT flag are selected. For each event, timestamp, runnumber and event number are extracted into a text file.The raw CMT data is converted to aROOT file for each run. An iteration over both85
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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
Page 42 and 43: Table 3.4: Data structure for calib
Page 44 and 45: TDC SpectrumN/[2 Channels]1000800H_
Page 46 and 47: Table 3.5: List of variables calcul
Page 48 and 49: with ∆⃗q = ⃗q n − ⃗q n−
Page 50 and 51: N [a.u.]∆ α (x)2200020000da0Entr
Page 52 and 53: d[mm]Reco Drift Distances201816H_RE
Page 54 and 55: N [a.u.]Real DataReal data0.06MCh1E
Page 56 and 57: χ 2N [a.u.]Probability103×10hc2p0
Page 58 and 59: N [a.u]Residuals20001800h0Entries 3
Page 60 and 61: 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 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 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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