Mohamad-Ziad Charif - Antares

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Anchor & BuoyEach line is anchored to the sea bed via a bottom string socket (BSS) , every BSSis as well equipped with a autonomous transponder that can help to position itselfwith reference to acoustic transponders located around the detector . Each lineis equipped with an anchor as well with a buoy, the role of the buoy is simply tohold the line straight. On a side note, the BSS of lines 7 and 8 hold a laser beaconwhich is use to do inter-line offset calibration, this will be discussed in the nextsection .3.2.1.2 CalibrationAs previously mentioned the LED’s and hydrophones installed on the stories andthe BSS’ are used to calibrate the detector. The ANTARES detector calibration isdivided into three separate but yet important calibration systems:Positioning and pointingIn order to accurately pinpoint astrophysical objects with reference to ANTARESa positioning and pointing calibration should be performed. This is done withthe LFLBL (Low Frequency Long BaseLine positioning system[91]) acoustic positioningsystem found on the BSS of every line. This system uses frequenciesbetween 8 and 16 KHz , this range of frequencies helps determine the overallposition of ANTARES by triangulation with five transponders located around thedetector with an addition of a ship positioned above the detector. With the help ofmore than 100 GPS positioning calculation done on the ship, an absolute positionof ANTARES relative to earth with an accuracy of 1 m and an accuracy of 1 ◦ and0.1 ◦ degrees in horizontal and vertical pointing.In addition to using the acoustic system to calibrate the pointing of ANTAREStwo other methods are implemented to independently verify the results.Moon ShadowAs the Moon rotates around Earth it will block cosmic rays (Figure 3.16), this willresults with fewer than expected number of down-going muons in the direction ofthe Moon. So one method of verifying the pointing of ANTARES is to look fora deviation of the deficit of down-going muons in respect to the expected Moonposition for ANTARES. It is expected that with enough data (at least 5 years ) wewould be able to improve the horizontal pointing accuracy below 1 ◦ .48
Figure 3.15: The LFLBL system, measurements of distance are done between theBSS and the transponders, BSS and the ship, and between transponders and theship.Figure 3.16: Moon shadow with cosmic rays.49
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 52 and 53: Figure 3.17: Distribution of azimut
Page 54 and 55: Figure 3.20: Height and radial disp
Page 56 and 57: Figure 3.22: Distribution of sea cu
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
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a look at figure 5.22 we find a cle
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The resulting optimized sensitiviti
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Figure 5.26: A comparison plot of t
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dΦ µdE ν= dΦ νdE νP earth ρN
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Figure 5.31: Limits on the muon flu
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Chapter 6Dark Matter search in the
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Figure 6.1: . True Position of the
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Figure 6.3: Comparison of the three
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For BBFit all variables mentioned i
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Figure 6.6: The distribution of χ
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annihilation channel W + W − the
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lowering the total contribution of
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6.4.2 BBFit Single-line analysisThe
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Figure 6.15: Comparison between the
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Figure 6.17: Comparison of Nhit dis
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Figure 6.19: The estimation of the
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Figure 6.21: Comparison of the opti
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Figure 6.23: Comparison of sensitiv
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Figure 6.25: Estimation of our back
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Figure 6.28: Comparison of the mult
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Figure 6.29: Comparison of the Λ d
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Figure 6.31: Comparison of the cos(
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Figure 6.34: Comparison of the esti
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The optimal Λ cut for all dark mat
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Figure 6.40: Sensitivity to neutrin
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6.7 Comparison with 2007-2008 analy
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mass of 200 GeV and a cross-section
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Chapter 7ConclusionsThe limits pres
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Bibliography[1] Volders, L. M. J. S
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[22] S. Burles et al., “Big bang
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[46] G. Debrassi, S. Heinemeyer, W.
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[74] C. Hettlage, K. Mannheim, and
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[102] D. Heck and J. Knapp, “Fors
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Mohamad-Ziad Charif - Antares

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