Muon Vertical Depth Intensity Distribution at the South Pole with AMANDA-II Kimberly Moody 1 August...
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Muon Vertical Depth Intensity Distribution at the South Pole with AMANDA-II Kimberly Moody 1 August 2003
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Transcript of Muon Vertical Depth Intensity Distribution at the South Pole with AMANDA-II Kimberly Moody 1 August...
Muon Vertical Depth Intensity Distribution at the South Pole
with
AMANDA-II
Kimberly Moody1 August 2003
Meet AMANDA-IIAntarctic Muon And Neutrino Detector Array
Located at the Geographic South Pole
677 Optical Modules (OMs) arranged on 19 strings
1500 to 2000m below the surface
AMANDA is a neutrino telescope...
The Beauty of Neutrinos
Protons deflected...
Photons interacting with cosmic background...
The neutrino remains unaffected!
Black Hole, Gamma Ray Burst
What kind of signal does AMANDA receive?
Diffuse Cosmic Rays (well-modeled)interact with atmosphere to produce, among other things, low energy muons.
What kind of signal does AMANDA receive?
Diffuse Cosmic Rays
Prompt Muons (different models suggest different fluxes; the subject of my research)
What kinds of signals does AMANDA receive?
Diffuse Cosmic Rays
Prompt Muons
High-Energy Neutrinos-bingo!-the tell-tale particles AMANDA is looking for.
Atm
osph
ere
High EnergyExtraterrestrialNeutrino
High Energy Prompt Muon (from charmed meson decay)
Low Energy Conventional Muons(from kaon and pion decay)
Convention Muons (absorbed by Earth)
Signals
Atmospheric Neutrino
This way up.
Data versus Monte Carloand Quality Criteria
Data versus Monte Carloand Quality Criteria
Slant Depth
173
0m
8650m
1 2 3 45
67
8
Slant Depth BinningBin=1730/cos θ
Prompt MuonsRQPM, QGSM: Most Optimistic Models
Graph: Gelmini, Gondolo, Varieschi Measuring the prompt atmospheric neutrino flux with down-going muons in neutrinos telescopes (2002) hep-ph/0209111
The Results of Our Prompt Muon Search
Prompt Contamination in First BinsR=Npm/Nmc
R(2)
= 0.106 %R(1)
= 0.0765 %
Bin 1 Bin 2
Prompt Muon Contamination in Last Bins R=Npm/Nmc
Bin Seven Bin Eight
R(8)
=1.55 %R(7)
=0.982 %
cos θ cos θ
cos θ cos θ
Inte
nsit
y by
bin
, cm
-2s-1
sr-1
Bin 1 Bin 2
Bin 3 Bin 4
Inte
nsit
y by
bin
, cm
-2s-1
sr-1
cos θ cos θ
cos θ cos θ
Bin 5 Bin 6
Many Thanks To:
National Science Foundation
The AMANDA Collaboration
Fellow Charlie's Angels
Dr. Bob Benjamin
Dr. Paolo Desiati
