19. April, 2004, Udine Workshop Keiichi Mase

Results from an Analysis of Muon Rings

Keiichi Mase

19. April, 2004, Udine Workshop Keiichi Mase

• Length of the arc ~ θc x D/R• Image Size(Total photons) ~ sin2 θc x 1/tan θc x D/R ~ θc x D/R → Good correlation between Arc Len. and SIZE

Muon images is simply determined by the geometryMuon images is simply determined by the geometry

θc

Impact parameter (R)

Mirror diameter (D)

Impact parameter (R) θc

Muons

19. April, 2004, Udine Workshop Keiichi Mase

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Observed Muon Events

19. April, 2004, Udine Workshop Keiichi Mase

Information from MuonsRun#17036 Event#794 Radius : 1.17 deg. Arc Len. : 4.05 deg. Arc Phi : 198 deg. Arc Wid. : 0.0951 deg. Est. I.P. : 4.92 m Mu SIZE : 5742 ADC

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19. April, 2004, Udine Workshop Keiichi Mase

Muon Selection Criteria

• 0.6 < Rad. < 1.3 deg.

• 0.03 < Arc Wid. < 0.16 deg.

• Arc Phi > 90 deg.

• Mu SIZE > 2000 ADC

• 1 < χarc phi2 < 10

• 1 < χarc wid2 < 10

Correct muon ratio ~95% (Arc Phi > 180 deg.)

• Random Forest Method may be better solution.

19. April, 2004, Udine Workshop Keiichi Mase

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Arc Width

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Real Data (27, Jan., 2004)

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Real Data (15, Feb., 2004)

MC (Original) MC (Spread)

19. April, 2004, Udine Workshop Keiichi Mase

Calibration with Muons

• Comapre the muon SIZE of Data (ADC) with one of MC (ph.e.).• The correction of MC is done.

• Mirror area (MC:240m2, Data:200m2)• Mirror reflectivity (MC: 85%, Data: 80%)• Plexiglas (MC: 100%, Data: 92%)• Collection eff. (MC: 100%, Data: 90%)• Light guide (MC: 100%, Data: 90%)

• Convphe→ADC = 0.26±0.05 ph.e./ADC

(c.f. F-factor method: Convphe→ADC = 0.17±0.02 ph.e./ADC)• Bugs (Not correctly flat-fielded) Conv. Factor from muons will become small. (0.21±0.04 ph.e./ADC?)

MC

Data

19. April, 2004, Udine Workshop Keiichi Mase

Muon Rates

• Use only one run (Run#17036 (ZA: 29.5 deg.) from 15, Feb.) (not systematical study)

• I put stronger condition of “Arc Phi > 180 deg.” (big arcs)

• 28/16870(0.17%) x 167 Hz = 0.28 Hz from Data

• 51/25668(0.20%) x 380 Hz = 0.76 Hz from MC (spread proton)

Low muon rate (only 37%)

• Missing low energy muon?• Detection eff. is low for real data?

19. April, 2004, Udine Workshop Keiichi Mase

Monitoring the Telescope

Correlation?

Arc Width Humidity

19. April, 2004, Udine Workshop Keiichi Mase

Summary

• Software is ready → I will commit them during this workshop.• Muons are correctly extracted. (~95%).

• The cuts to extract muons should be optimised (option: Random Forest method)• The detection efficiency of muons should be evaluated.

• The conversion factor from ADC to ph.e. is roughly consistent between muon and F-factor method. However, the small difference should be investigated more (, fixing my bugs). The treatment of bad pixels will be important.

• Observed muon rates is lower than MC (~40%).

• The monitoring telescope by muon should be done (, taking the correlation with the weather condition).

19. April, 2004, Udine Workshop Keiichi Mase

Back up

19. April, 2004, Udine Workshop Keiichi Mase

Muon images

• With increasing impact parameter, • and because of coma aberration, The image of a muon becomes more similar to that of a gamma.

γ image(30GeV)

19. April, 2004, Udine Workshop Keiichi Mase

Lateral distribution from a single muon

MAGIC will observe many muons because of the large collection area and its high sensitivity.