Mohamad-Ziad Charif - Antares

More documents

Recommendations

Info

Figure 3.22: Distribution of sea current speed (on the left) and its horizontal direction(right).The Onshore calibration of the OMs offset (Figure3.24 ) is done in a darkroom to eliminate unwanted light sources. A controlled laser beam is sent to theOM as seen in figure 3.23 . The offset is calculated in reference to the first OM ofthe first floor.The in situ calibrationon the sea bed.is actually a set of three different calibrations done• Using the LED beacons[93] the OM offset can be recalculated (Figure 3.24) using these beacons that flashes light at λ = 470 nm. These beacons existon floors 2, 9 , 15, and 21 of each line. This is done by flashing the LEDbeacons and measuring the time differences of the signal among the differentOMs and a reference OM. However, since the first LED beacon is on thesecond floor of each line, the offset can not be measured for the first flooras the light from the LED is emitted upwards, this is solved using the laserbeacons.• Using the laser beacon[93] on the BSS of lines 8. This laser beacon whichflashes laser beams at λ = 532 nm can calculate the inter-line offset betweenall lines and line 8. This is done as well by flashing the laser beacon andmeasuring the time differences of the signal among the different lines. Inaddition, the laser beacon can measure the OM offset for the first floors ofeach line as as the laser beacon is placed below the first floor.• 40 K which occurs naturally in sea water, it is a radioactive isotope of Potassium.The decay of 40 K can produce photons which can help in an indepen-54
Figure 3.23: OM time offset calibration setup as done in a dark room.dent way calibrate the arrival time of photons (Figure 3.25). This is done bystudying hits coincidence on two adjacent OMs (Figure 3.26).The various methods used to do the time calibration of the detector achieve anaccuracy less than 1 ns.Angular resolutionThe eventual precision of ANTARES is measured by the value of the angle betweenthe trajectory of the neutrino and the reconstructed muon trajectory whichis very much dependent on the time calibration and knowing the precise locationof every OM, in addition to depending on the kinematics of ν → µ + X .55
Page 2 and 3:
"The most exciting phrase to hear i
Page 4 and 5:
3.2.1.4 Performance and characteris
Page 6 and 7: Chapter 1IntroductionThe early hist
Page 8 and 9: Chapter 2Dark MatterIn this chapter
Page 10 and 11: Figure 2.2: Comparison of the measu
Page 12 and 13: Figure 2.4: CMB anisotropy observed
Page 14 and 15: Figure 2.5: Combination of the WMAP
Page 17: Figure 2.6: Temporal evolution of t
Page 20 and 21: Figure 2.9: Parameter space of m 1/
Page 22 and 23: Figure 2.10: Limits on spin-indepen
Page 26 and 27: Figure 2.14: Detected gamma ray flu
Page 28 and 29: 600km/s. If we assume the worst cas
Page 30 and 31: Figure 2.17: Conversion factor from
Page 32 and 33: The eigenstate mixing can be writte
Page 34 and 35: Figure 2.19: Flux of ν µ / ¯ν
Page 36 and 37: Figure 3.1: The neutral current (NC
Page 38 and 39: Muon Energy (GeV )1p| dEdx | (GeV.c
Page 40 and 41: Figure 3.4: Energy loss of per dist
Page 42 and 43: Figure 3.6: Effective muon range as
Page 44 and 45: Figure 3.8: Differential flux of at
Page 46 and 47: 3.2.1.1 Detector layoutOptical Modu
Page 48 and 49: • The LED (light emitting diode)
Page 50 and 51: Anchor & BuoyEach line is anchored
Page 52 and 53: Figure 3.17: Distribution of azimut
Page 54 and 55: Figure 3.20: Height and radial disp
Page 58 and 59: Figure 3.24: Time offset among OMs
Page 60 and 61: Figure 3.26: Distribution of time d
Page 62 and 63: Line number Connection Date Mainten
Page 64 and 65: Figure 3.29: Comparison between sky
Page 66 and 67: Figure 3.31: The effective area for
Page 68 and 69: Figure 4.1: Median counting rate of
Page 70 and 71: Figure 4.4: Average neutrino events
Page 72 and 73: 2. All hits on the same floor are m
Page 74 and 75: 4.2.1 Neutrino simulationFigure 4.6
Page 76 and 77: • Multiplicity range of the muon
Page 78 and 79: Chapter 5Dark Matter search in the
Page 80 and 81: Figure 5.2: Annihilation spectrum f
Page 82 and 83: Livetime(days) 5 Lines 9 Lines 10 L
Page 84 and 85: Figure 5.4: Monte Carlo Truth distr
Page 86 and 87: Figure 5.7: Tchi2 distribution for
Page 88 and 89: Figure 5.9: Tchi2 distribution for
Page 90 and 91: Figure 5.11: Sun’s position taken
Page 92 and 93: Figure 5.13: Comparison between the
Page 94 and 95: Figure 5.15: Estimation of the back
Page 96 and 97: Figure 5.16: Mean angle between the
Page 98 and 99: Figure 5.18: A comparison of the di
Page 100 and 101: a look at figure 5.22 we find a cle
Page 102 and 103: The resulting optimized sensitiviti
Page 104 and 105: Figure 5.26: A comparison plot of t
Page 106 and 107:
dΦ µdE ν= dΦ νdE νP earth ρN
Page 108 and 109:
Figure 5.31: Limits on the muon flu
Page 110 and 111:
Chapter 6Dark Matter search in the
Page 112 and 113:
Figure 6.1: . True Position of the
Page 114 and 115:
Figure 6.3: Comparison of the three
Page 116 and 117:
For BBFit all variables mentioned i
Page 118 and 119:
Figure 6.6: The distribution of χ
Page 120 and 121:
annihilation channel W + W − the
Page 122 and 123:
lowering the total contribution of
Page 124 and 125:
6.4.2 BBFit Single-line analysisThe
Page 126 and 127:
Figure 6.15: Comparison between the
Page 128 and 129:
Figure 6.17: Comparison of Nhit dis
Page 130 and 131:
Figure 6.19: The estimation of the
Page 132 and 133:
Figure 6.21: Comparison of the opti
Page 134 and 135:
Figure 6.23: Comparison of sensitiv
Page 136 and 137:
Figure 6.25: Estimation of our back
Page 138 and 139:
Figure 6.28: Comparison of the mult
Page 140 and 141:
Figure 6.29: Comparison of the Λ d
Page 142 and 143:
Figure 6.31: Comparison of the cos(
Page 144 and 145:
Figure 6.34: Comparison of the esti
Page 146 and 147:
The optimal Λ cut for all dark mat
Page 148 and 149:
Figure 6.40: Sensitivity to neutrin
Page 150 and 151:
6.7 Comparison with 2007-2008 analy
Page 152 and 153:
mass of 200 GeV and a cross-section
Page 154 and 155:
Chapter 7ConclusionsThe limits pres
Page 156 and 157:
Bibliography[1] Volders, L. M. J. S
Page 158 and 159:
[22] S. Burles et al., “Big bang
Page 160 and 161:
[46] G. Debrassi, S. Heinemeyer, W.
Page 162 and 163:
[74] C. Hettlage, K. Mannheim, and
Page 164:
[102] D. Heck and J. Knapp, “Fors
show all

Mohamad-Ziad Charif - Antares

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

Delete template?

Save as template?