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

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

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

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

Muon Spectrum Muon Energy Spectrum Patrick Berghaus

Pion Production Pion Energy LHC 1 TeV Primary Nucleon Energy G.D. Barr, T.K. Gaisser, S. Robbins, T. Stanev, astro-ph/0611266 Muon Energy Spectrum Patrick Berghaus

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

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

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

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

CASKADE Composition Measurement Muon Energy Spectrum Patrick Berghaus astro-ph/0505413 Muon Energy Spectrum Patrick Berghaus

CR Composition and Muon Energy Muon Energy Spectrum Patrick Berghaus

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

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

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

Slant Depth and Bundle Multiplicity Muon Energy Spectrum Patrick Berghaus

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

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

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

Slant Depth Zenith Angle diff int Muon Energy Spectrum Patrick Berghaus

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

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

CR Energy Credit: Keiichi Muon Energy Spectrum Patrick Berghaus

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

Zenith Angle ±0.1% Muon Energy Spectrum Patrick Berghaus

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

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

Slant Depth ±3% Muon Energy Spectrum Patrick Berghaus

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

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

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

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

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

(Qtot / Npulse) Muon Energy Spectrum Patrick Berghaus

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

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

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

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

Average Charge per Pulse Invariant! Muon Energy Spectrum Patrick Berghaus

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

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

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

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

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

Muon Spectrum Muon Energy Spectrum Patrick Berghaus

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

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

Backup Slides Muon Energy Spectrum Patrick Berghaus

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

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

Muon Energy Spectrum Patrick Berghaus

Muon Energy Spectrum Patrick Berghaus

Muon Energy Spectrum Patrick Berghaus

Muon Energy Spectrum Patrick Berghaus

Muon Energy Spectrum Patrick Berghaus