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

More documents

Recommendations

Info

Lateral x Resolution CMT - IDhlatx_idLateral y Resolution CMT - IDhlaty_idEntries 82Entries 82number of entries [per 0.2m]12108Mean 0.05097RMS 2.628norm 13.03 ±0.99mean -0.452 ±0.056σ 0.668 ±0.062number of entries [per 0.2m]16141210Mean 0.06291RMS 1.996norm 9.754 ±0.677mean -0.1656 ±0.0250σ 0.3403 ±0.032568644220-10 -8 -6 -4 -2 0 2 4 6 8 10∆ x [m]0-10 -8 -6 -4 -2 0 2 4 6 8 10∆ y [m]Figure 5.22: Lateral resolution ∆x and ∆y from the comparison of CMT and IDtrackingImpact parameter CMT and BX-GL Tracks22hi_glEntries 125Mean 0.383220RMS 1.06618norm 19.31±0.7616mean 0.1749 ±0.0204σ 0.466 ±0.02414number of entries [per 0.2m]121086420-4 -3 -2 -1 0 1 2 3 4∆ I [m]Figure 5.23: Lateral resolution of the impact parameter I from the comparison ofCMT and global tracking. The slight shift of the distribution is explained by the fact,that the impact parameter of tracks reconstructed by the CMT can lie outside of theactual Borexino vessel and can thus obtain larger values.90
zyI 1I 2d Ixµ 2µ 1Figure 5.24: Example of relative positions of the reconstruction of a muon track byboth the CMT and Borexino in the coordinate system of the SSS. I is the impactparameter of each track. For the determination of the lateral resolution, the distanced I (green line) between the points closest to the center for each track is calculated.trackings does not take into account their relative position. To study this effect, theclosest point to the center of the SSS of the tracks reconstructed by Borexino andthe CMT have been determined as shown in Fig. 5.24 and the distances d I betweenthem have been calculated. The distribution of d I is depicted in Fig. 5.25 for theBorexino global tracking. A clear peak can be seen with a mean value of ¯d I givinga measure of the lateral resolution. All methods lead to a lateral resolution around50 cm with the results using the impact parameter comparison being slightly betterand more consistent than the other ones.5.5 CNGS Rock MuonsThe CMT is based on the drift tube technology developed for the OPERA detector.OPERA searches for ν τ appearance in a ν µ beam [79]. The CNGS 2 ν µ -beam isgenerated as described in Section 2.4.6 at a distance of 732 km from Gran Sasso atCERN, focused on the Hall C where both OPERA and Borexino are located. Thebeam travels through the Earth before it arrives at Gran Sasso at an inclinationof approximately -3.5 ◦ [80]. Neutrinos in the CNGS beam have a mean energy of17 GeV. Although the cross section for neutrino interactions is rather small, some2 CNGS CERN Neutrinos to Gran Sasso91
Page 1 and 2:
Setup of a Drift Tube Muon Trackera
Page 3:
AbstractIn this work the setup and
Page 6 and 7:
3.5.5 Pattern Recognition . . . . .
Page 8 and 9:
viii
Page 10 and 11:
essential for vetoing these events.
Page 13 and 14:
Chapter 2NeutrinosThe standard mode
Page 15 and 16:
However, it did not yet deliver an
Page 17 and 18:
Table 2.1: Neutrino oscillation par
Page 19 and 20:
this assumption, the Standard Solar
Page 21 and 22:
Figure 2.1: Neutrino flux at Earth
Page 23 and 24:
asymmetry between neutrino and anti
Page 25 and 26:
Figure 2.3: Expected ¯ν e energy
Page 27:
Nb neutrino/fission-11010-2Neutrino
Page 30 and 31:
108−dE/dx (MeV g −1 cm 2 )65432
Page 32 and 33:
Figure 3.3: Setup of the muon track
Page 34 and 35:
zyxModule b.0Module a.0Module b.1Mo
Page 36 and 37:
Figure 3.6: Display of the slow con
Page 38 and 39:
plastic scintillators. To avoid all
Page 40 and 41:
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 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 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
Page 124 and 125: 116
Page 126: Jan Lenkeit und Björn Wonsak sowie
show all

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

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?