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

More documents

Recommendations

Info

N [arbitrary units]∆y all data20018016014012010080604020σ t= 0.962677h10Entries 1924Mean -0.04302RMS 1.668c 384.8 ± 9.0σ 0.3411 ± 0.0542lg 0.9739 ± 0.0624shift 0.0005585 ± 0.02038920-10 -8 -6 -4 -2 0 2 4 6 8 10∆ y [m]N [arbitrary units]∆ z all data18016014012010080604020σ t= 1.125102h11Entries 1924Mean 0.0002146RMS 1.808c 368.6 ± 8.9σ 0.6724 ± 0.0617lg 0.8252 ± 0.0799shift -0.03227 ± 0.026840-10 -8 -6 -4 -2 0 2 4 6 8 10∆ z [m]∆y p>50GeVN [arbitrary units]35σ30 t= 0.5131612520h12Entries 192Mean 0.02569RMS 1.208c 38.37 ± 3.18σ 0.2829 ± 0.0758lg 0.4082 ± 0.1600shift 0.008391 ± 0.038067Delta z p>50 GeVN [arbitrary units]30 σ t= 0.8276962520h13Entries 192Mean 0.2856RMS 1.83c 38.42 ± 2.99σ 0.001092 ± 0.000374lg 0.9726 ± 0.1232shift 0.02499 ± 0.0470815151010550-10 -8 -6 -4 -2 0 2 4 6 8 10∆ y [m]0-10 -8 -6 -4 -2 0 2 4 6 8 10∆ z [m]∆y, p>20GeV, nhits>7000N [arbitrary units]40σ t= 0.3766443530252015h14Entries 195Mean 0.01924RMS 1.444c 36.63 ± 2.81σ 0.2204 ± 0.0468lg 0.2826 ± 0.0863shift 0.09905 ± 0.02760∆z, p>20GeV, nhits>7000N [arbitrary units]35 σ t= 0.55297730252015h15Entries 195Mean 0.3447RMS 2.104c 36.59 ± 3.06σ 0.1772 ± 0.1693lg 0.5755 ± 0.1972shift -0.004885 ± 0.0376591010550-10 -8 -6 -4 -2 0 2 4 6 8 10∆ y [m]0-10 -8 -6 -4 -2 0 2 4 6 8 10∆ z [m]Figure 5.31: Spatial resolution of the Borexino muon reconstruction. The totalresolution σ t is derived from the FWHM98
Chapter 6Summary and OutlookThe spectroscopic real time detection of low energetic 7 Be solar neutrinos has recentlybeen achieved for the first time by the Borexino experiment. Together withthe measurement of the 8 B solar neutrino flux, the borders of the transition regionbetween 1 and 10 MeV of the MSW effect could now be addressed by a single experimentsupporting the model of matter enhanced oscillations. The experimentaldetermination of the solar neutrino fluxes resulting from different fusion processesin the Sun allows to test the input parameters of the SSM such as the metallicity orsolar composition.7 Be and 8 B neutrinos mainly cover the borders of the transition region of theMSW effect. A measurement of the flux of solar neutrinos with intermediate energiesaround 1 MeV would allow to give further constraints on the different models for solarneutrino oscillations in matter. Whereas the MSW-LMA model seems to be favoredby Borexino in combination with the other solar oscillation experiments, recentanalyses including also the KamLAND data see hints for possible non standardinteractions.Neutrinos from the pep and CNO solar fusion processes cover the intermediateenergies in the transition region. Measuring for the first time the flux of CNOneutrinos would also allow for the determination of the contribution of the CNO cycleto the energy production in the Sun. However, in Borexino their energy regime isdominated by the uncorrelated decays of cosmogenic induced 11 C nuclei by at leastone order of magnitude. To distinguish these decays from the neutrino signal, aprecise tracking of the incident muons is necessary. For the Borexino experiment,a sophisticated muon tracking procedure based on the PMT timing information isused.The compact muon tracker presented in this work exceeds the performance ofthe Borexino tracking by far and can hence be used to test it. The CMT has beenbuilt from drift tube modules formerly used for calibration measurements for theOPERA experiment. A modification of the setup done within this thesis allows fora precise three dimensional reconstruction of muon tracks. An independent slowcontrol software based on Linux has been developed, allowing a remote control ofall detector components via a simple terminal connection. A new software packagefor alignment, calibration, and event processing including 3D track reconstructionhas been introduced. With the CMT setup, an angular resolution of 4.65 mrad anda spatial resolution of 270ñm have been reached.99
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 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 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?