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

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[49] T. Araki et al. Experimental investigation of geologically produced antineutrinoswith KamLAND. Nature, 436:499–503, 2005.[50] G. Bellini et al. Observation of Geo-Neutrinos. Phys. Lett., B687:299–304,arXiv:1003.0284.[51] Gianni Fiorentini, Marcello Lissia, and Fabio Mantovani. Geo-neutrinos andEarth’s interior. Phys. Rept., 453:117–172, arXiv:0707.3203.[52] F. Ardellier et al. Letter of intent for double-CHOOZ: A search for the mixingangle theta(13). arXiv:hep-ex/0405032.[53] Edda Gschwendtner. CERN neutrinos to Gran Sasso (CNGS): First beam.Prepared for 2006 IEEE Nuclear Science Symposium (NSS), Medical ImagingConference (MIC) and 15th International Room Temperature SemiconductorDetector Workshop, San Diego, California, 29 Oct - 4 Nov 2006.[54] D. Drakoulakos et al. Proposal to perform a high-statistics neutrinoscattering experiment using a fine-grained detector in the NuMI beam.arXiv:hep-ex/0405002.[55] Y. Itow et al. The JHF-Kamioka neutrino project. arXiv:hep-ex/0106019.[56] Claude Amsler et al. Review of particle physics. Phys. Lett., B667:1, 2008.[57] F. Sauli. Principles of Operation of Multiwire Proportional and Drift Chambers.CERN-77-09.[58] R. Zimmermann et al. The precision tracker of the OPERA detector. Nucl.Instrum. Meth., A555:435–450, 2005.[59] P. Reviersma. The l3 wire - amplifier. 1986. NH19-6112.[60] R. van Staa J. Schütt. OSUB OPERA Supportboard. Universität Hamburg,Institut für Experimentalphysik, February 2006.[61] R. van Staa J. Schütt. OTB OPERA Triggerboard. Universität Hamburg,Institut für Experimentalphysik, March 2006.[62] Klaus Hitschler Peak System-Technik GmbH. PCAN-driver for Linux, 2007.[63] MSC Vertriebs GmbH. Benutzerhandbuch DES OPERA, 2004. in German.[64] C. Girerd. OPERA TDC controller board Test Acquisition Tools Getting startedManual, 2006.[65] I.N. Bronstein, K.A. Semendjajew, G. Musiol, and H. Mühlig. Taschenbuch derMathematik. Verlag Harry Deutsch, Thun und Frankfurt am Main, 5 edition,2001.[66] R. K. Bock, (Ed. ), K. Bos, (Ed. ), S. Brandt, (Ed. ), J. Myrheim, (Ed. ),and M. Regler, (Ed. ). FORMULAE AND METHODS IN EXPERIMENTALDATA EVALUATION WITH EMPHASIS ON HIGH-ENERGY PHYSICS.VOL. 3: ARTICLES ON STATISTICAL AND NUMERICAL METHODS. PetitLancy, Switzerland: Eps ( 1984) Nonconsec. Pag.114
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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
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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 120 and 121: [14] Ch. Kraus et al. Final Results
Page 124 and 125: 116
Page 126: Jan Lenkeit und Björn Wonsak sowie
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