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IceCube Collaboration Meeting

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Presentation on theme: "IceCube Collaboration Meeting"— Presentation transcript:

1 IceCube Collaboration Meeting
Muon Energy Spectrum Patrick Berghaus IceCube Collaboration Meeting Spring 2009

2 Detector Calibration High Statistics from atmospheric muons
Distributions near the horizon sensitive to: Zenith Angle Resolution Misreconstructed Background High-Energy Events Systematics discovered in the course of this analysis: See PB talk in Muon Session Muon Energy Spectrum Patrick Berghaus

3 Diffuse Analyses High-Energy Events
Validity of lepton production models CR composition effects Muon Energy Spectrum Patrick Berghaus

4 CR Physics CR composition Hadron production in nn interactions
Air Shower Models Muon Energy Spectrum Patrick Berghaus

5 Muon Spectrum Muon Energy Spectrum Patrick Berghaus

6 Pion Production Pion Energy LHC 1 TeV Primary Nucleon Energy
G.D. Barr, T.K. Gaisser, S. Robbins, T. Stanev, astro-ph/ Muon Energy Spectrum Patrick Berghaus

7 Knee:≃3PeV 2nd Knee:≃40PeV Ankle:≃3EeV g≃-2.7 g≃-3.0 g≃-3.2 g≃-2.4-2.7
Muon Energy Spectrum Patrick Berghaus

8 Gyroradius: “Leaking Box” Fe p Muon Energy Spectrum Patrick Berghaus

9 Extended Air Shower Measurements:
Altitude of Shower Maximum Composition Change at ≥few PeV Shower Maximum Muon Energy Spectrum Patrick Berghaus

10 poly-gonato (Hoerandel) Rigidity Mass Constant astro-ph/0210453
Muon Energy Spectrum Patrick Berghaus

11 CASKADE Composition Measurement Muon Energy Spectrum Patrick Berghaus
astro-ph/ Muon Energy Spectrum Patrick Berghaus

12 CR Composition and Muon Energy
Muon Energy Spectrum Patrick Berghaus

13 Prompt Muons: Out of Reach!
Conventional Muons (near horizon) 1PeV Muon Energy Spectrum Patrick Berghaus

14 Calorimetric Response for Bundles
Source: Dima minimum ionizing Muon Energy Spectrum Patrick Berghaus

15 Slant Depth 1.5km 2.5km (283GeV) (1.12TeV) 10km (81°) 10km (74°)
Muon Energy Spectrum Patrick Berghaus

16 Slant Depth and Bundle Multiplicity
Muon Energy Spectrum Patrick Berghaus

17 Dqzen “Good” Muons “Bad” Muons Muon Energy Spectrum Patrick Berghaus

18 L3 Cuts 0: qzen,llh>70° && muonfilter 1: Nchan>15
2: sparab<6° 3: llhred(2.5)<8 4: Ylf,llh<0.2rad 5: 100m<Ldir(C)<800m 6: 0.15<vlf<0.4 && abs(smooth)<0.6 wiki.icecube.wisc.edu/index.php/Muon_Energy_Spectrum/Level_3 Muon Energy Spectrum Patrick Berghaus

19 Final Cut Level Cut 0: llhred(2.5)<7.25
Cut 1: llhred(2.5)<7.1 sparab,zen<2° Cut 2: llhred(2.5)<7.0 sparab,zen<1.4° Final Cut Level wiki.icecube.wisc.edu/index.php/Muon_Energy_Spectrum/Final_Cuts Muon Energy Spectrum Patrick Berghaus

20 Slant Depth Zenith Angle diff int Muon Energy Spectrum
Patrick Berghaus

21 Total Charge True Zenith “Reference Cut”: From All-Sky Analysis
Neutrinos True Zenith Muon Energy Spectrum Patrick Berghaus

22 ∣True Zenith – Reconstructed Zenith∣
no tracks in tail Muon Energy Spectrum Patrick Berghaus

23 CR Energy Credit: Keiichi Muon Energy Spectrum Patrick Berghaus

24 Highest Muon Energy in Shower (at surface) Muon Energy Spectrum
Patrick Berghaus

25 Zenith Angle ±0.1% Muon Energy Spectrum Patrick Berghaus

26 Slant Depth: Correction true slant depth measured slant depth
Muon Energy Spectrum Patrick Berghaus

27 Slant Depth 50 TeV Track Multiplicity in Detector Max. Muon Surface
Energy Muon Energy Spectrum Patrick Berghaus

28 Slant Depth ±3% Muon Energy Spectrum Patrick Berghaus

29 Data/MC: Slant Depth Angular resolution too low
to go further, better in the future! 1 Muon Energy Spectrum Patrick Berghaus

30 Pulses (Qtot similar) Track Multiplicity in Detector Max. Muon Surface
High-Multiplicity Bundles Track Multiplicity in Detector Pulses (Qtot similar) Max. Muon Surface Energy Muon Energy Spectrum Patrick Berghaus

31 Pulses “Elbert-Formula” 2.5-3 times more muons for Fe than p
Muon Energy Spectrum Patrick Berghaus

32 Total Charge “Elbert-Formula” 2.5-3 times more muons for Fe than p
Muon Energy Spectrum Patrick Berghaus

33 Data/MC: Npulse and Qtot
1 Muon Energy Spectrum Patrick Berghaus

34 (Qtot / Npulse) Muon Energy Spectrum Patrick Berghaus

35 Surface Energy Estimator 200 TeV Track Multiplicity in Detector
Max. Muon Surface Energy Muon Energy Spectrum Patrick Berghaus

36 Energy of most energetic
muon in shower by ẽ-bin unit area linear scale events per second logarithmic scale Muon Energy Spectrum Patrick Berghaus

37 Data/MC: ẽ(Npulse) and ẽ(Qtot)
1 Muon Energy Spectrum Patrick Berghaus

38 Data ẽ(pulse) ẽ(charge) MC Muon Energy Spectrum Patrick Berghaus

39 Average Charge per Pulse Invariant! Muon Energy Spectrum
Patrick Berghaus

40 Additional Cut: Average Charge per Pulse < 3
“Balloon”/Droop Correction Additional Cut: Average Charge per Pulse < 3 1 Muon Energy Spectrum Patrick Berghaus

41 Data/MC: ẽ(Npulse) and ẽ(Qtot)
1 Muon Energy Spectrum Patrick Berghaus

42 Data/MC: Npulse and Qtot
1 1 Muon Energy Spectrum Patrick Berghaus

43 Final Distribution (1 month IC22)
Expect 10 events in IC22 for const.comp. Muon Energy Spectrum Patrick Berghaus

44 Ratio Data/MC (1 month IC22)
Muon Energy Spectrum Patrick Berghaus

45 Muon Spectrum Muon Energy Spectrum Patrick Berghaus

46 Muon Spectrum IC22 (1month), PRELIMINARY! Muon Energy Spectrum
Patrick Berghaus

47 Conclusion Atmospheric muons are indispensable for
investigation of detector systematics Diffuse analysis is very difficult without understanding HE muons IceCube has huge potential for CR physics More information: wiki.icecube.wisc.edu/index.php/Muon_Energy_Spectrum Muon Energy Spectrum Patrick Berghaus

48 Backup Slides Muon Energy Spectrum Patrick Berghaus

49 cogz<-100m: ẽ(Npulse) and ẽ(Qtot)
Muon Energy Spectrum Patrick Berghaus

50 cogz<-100m: Npulse and Qtot
Muon Energy Spectrum Patrick Berghaus

51 Muon Energy Spectrum Patrick Berghaus

52 Muon Energy Spectrum Patrick Berghaus

53 Muon Energy Spectrum Patrick Berghaus

54 Muon Energy Spectrum Patrick Berghaus

55 Muon Energy Spectrum Patrick Berghaus

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