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Muon Vertical Depth Intensity Distribution at the South Pole with AMANDA-II Kimberly Moody 1 August 2003.

Published byMelinda Conley Modified over 9 years ago

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Presentation on theme: "Muon Vertical Depth Intensity Distribution at the South Pole with AMANDA-II Kimberly Moody 1 August 2003."— Presentation transcript:

1 Muon Vertical Depth Intensity Distribution at the South Pole with AMANDA-II Kimberly Moody 1 August 2003

2 Meet AMANDA-II Antarctic 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...

3 The Beauty of Neutrinos Protons deflected... Photons interacting with cosmic background... The neutrino remains unaffected! Black Hole, Gamma Ray Burst

4 What kind of signal does AMANDA receive? Diffuse Cosmic Rays (well-modeled) interact with atmosphere to produce, among other things, low energy muons.

5 What kind of signal does AMANDA receive? Diffuse Cosmic Rays Prompt Muons (different models suggest different fluxes; the subject of my research)

6 What kinds of signals does AMANDA receive? Diffuse Cosmic Rays Prompt Muons High-Energy Neutrinos-bingo!-the tell- tale particles AMANDA is looking for.

7 Atmosphere High Energy Extraterrestrial Neutrino 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.

8 Data versus Monte Carlo and Quality Criteria

9 Data versus Monte Carlo and Quality Criteria

10 Slant Depth 1730m 8650m 1 2 3 4 5 6 7 8 Slant Depth Binning Bin=1730/cos θ

11 Prompt Muons RQPM, 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

12 The Results of Our Prompt Muon Search

13 Prompt Contamination in First Bins R=N pm /N mc R (2) = 0.106 % R (1) = 0.0765 % Bin 1 Bin 2

14 Prompt Muon Contamination in Last Bins R=N pm /N mc Bin Seven Bin Eight R (8) =1.55 % R (7) =0.982 %

15 cos θ Intensity by bin, cm -2 s -1 sr -1 Bin 1 Bin 2 Bin 3 Bin 4

16 Intensity by bin, cm -2 s -1 sr -1 cos θ Bin 5Bin 6

17 Many Thanks To: National Science Foundation The AMANDA Collaboration Fellow Charlie's Angels Dr. Bob Benjamin Dr. Paolo Desiati

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