Muon Energy Spectrum
Transcript of Muon Energy Spectrum
Muon Energy Spectrum
Patrick BerghausIceCube Collaboration Meeting
Spring 2009
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Detector Calibration
High Statistics from atmospheric muonsDistributions near the horizon sensitive to:
Zenith Angle ResolutionMisreconstructed Background
HighEnergy Events
Systematics discovered in the course of this analysis:See PB talk in Muon Session
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Diffuse Analyses
HighEnergy EventsValidity of lepton production modelsCR composition effects
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CR Physics
CR compositionHadron production in nn interactionsAir Shower Models
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Muon Spectrum
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G.D. Barr, T.K. Gaisser, S. Robbins, T. Stanev, astroph/0611266
LHC
1 TeVPrimary Nucleon Energy
Pion
Ene
rgy
Pion Production
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Knee:≃3PeV
Ankle:≃3EeV
2nd Knee:≃40PeV≃2.7 ≃3.0
≃3.2
≃2.42.7
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p
Fe
Gyroradius:
“Leaking Box”
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Composition Change at ≥few PeV
Show
er M
axim
um
Extended Air Shower Measurements: Altitude of Shower Maximum
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Rigidity Mass Constant
polygonato(Hoerandel)
astroph/0210453
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astroph/0505413
CASKADE CompositionMeasurement
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≃3.7≃4.0
CR Composition and Muon Energy
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Prompt Muons: Out of Reach!
ConventionalMuons(near horizon)
1PeV
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Source: Dima
minimum ionizing
Calorimetric Response for Bundles
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1.5km(283GeV)
2.5km(1.12TeV) 10km (81°)
20km (85.5°)(38.6TeV)
20km (82°)
10km (74°)(4.88TeV)
Slant Depth
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Slant Depth and Bundle Multiplicity
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zen
“Good” Muons “Bad”
Muons
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0:zen,llh>70° && muonfilter1: Nchan>152:parab<6°3: llhred(2.5)<84: lf,llh<0.2rad5: 100m<Ldir(C)<800m6: 0.15<vlf<0.4 &&abs(smooth)<0.6
wiki.icecube.wisc.edu/index.php/Muon_Energy_Spectrum/Level_3
L3 Cuts
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Cut 0: llhred(2.5)<7.25Cut 1: llhred(2.5)<7.1 parab,zen<2°Cut 2: llhred(2.5)<7.0 parab,zen<1.4°
wiki.icecube.wisc.edu/index.php/Muon_Energy_Spectrum/Final_Cuts
FinalCut Level
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Slant Depth Zenith Angle
diff
int
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Total Charge
True Zenith
Neutrinos“Reference Cut”:From AllSky Analysis
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notracksintail
∣True Zenith – Reconstructed Zenith∣
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Credit: Keiichi
CR Energy
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HighestMuon Energyin Shower(at surface)
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Zenith Angle
±0.1%
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measured slant depth
true slant depth
Slant Depth:Correction
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Slant Depth
50 TeV
Track Multiplicityin Detector
Max. MuonSurfaceEnergy
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Slant Depth
±3%
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Data/MC: Slant Depth
1
Angular resolution too lowto go further, better in the future!
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Pulses(Q
tot similar)
HighMultiplicity BundlesTrack
Multiplicityin Detector
Max. MuonSurfaceEnergy
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Pulses
2.53 times more muons for Fe than p
“ElbertFormula”
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Total Charge
2.53 times more muons for Fe than p
“ElbertFormula”
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Data/MC: Npulse and Qtot
1
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(Qtot / Npulse)
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Surface Energy
Estimator
200 TeV
Track Multiplicityin Detector
Max. MuonSurfaceEnergy
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unit arealinear scale
events per secondlogarithmic scale
Energy of most energetic muon in shower
by ẽbin
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Data/MC: ẽ(Npulse) and ẽ(Qtot)
1
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ẽ(pulse)
ẽ(charge)
Data
MC
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Average Chargeper Pulse
Invariant!
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Additional Cut:Average Charge
per Pulse< 3
1
“Balloon”/Droop Correction
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Data/MC: ẽ(Npulse) and ẽ(Qtot)
1
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Data/MC: Npulse and Qtot
1 1
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Final Distribution (1 month IC22)
Expect 10 events in IC22
for const.comp.
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Ratio Data/MC (1 month IC22)
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IC22 (1month), PRELIMINARY!
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ConclusionAtmospheric 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
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Backup Slides
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cogz<100m: ẽ(Npulse) and ẽ(Qtot)
1 1
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cogz<100m: Npulse and Qtot
1 1
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