University of Wisconsin-Madison

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Presentation transcript:

University of Wisconsin-Madison The Angular Distribution of Atmospheric Muons in the AMANDA detector at a depth of 1730m Karen R. Bland Summer REU 2002 University of Wisconsin-Madison Madison, WI

Overview Introduction to AMANDA Atmospheric muons Analysis Results Some conclusions Future studies

Antarctic Muon and Neutrino Detector Array

Atmospheric Muons Produced by cosmic rays hitting atmosphere Background to neutrino analysis

Analysis Monte Carlo (MC) Same analysis is performed on MC and data: Simulation codes: Corsika, Corama, MMC, Amasim Data AMANDA-II (year 2000) data ~ 13,000 sec of lifetime (3.5 hrs) Same analysis is performed on MC and data: Hit cleaning Filtering Quality cuts

Quality Cuts Optimizing Removing mis-reconstructed events Angular resolution Data/MC response Stability

Cuts (cont’d) Cuts: Passing rates: MC: 62.5% Data: 56.0% Length of direct hits >120 m Track smoothness between –0.26 and +0.26 The time-likelihood fit reconstruction < 7.8 Passing rates: MC: 62.5% Data: 56.0%

Unfolding the detector data MC true zenith angle reconstructed zenith angle Data reconstructed zenith angle

Results: Angular Distribution Angular Distribution of Downgoing Muons at 1730 m Angular Distribution of Downgoing Muons at 1730 m S. Klimushin curve Data fit – 85 % MC fit – 68 % S.I. Sinegovsky curve Data fit – 73 % MC fit – 59 %

Results: Angular Distribution / Depth-Intensity Slant Depth Intensity of Down-going Muons Angular Distribution of Downgoing Muons at 1730 m

Results: MC-Data Response / Effective Area

Some conclusions Atmospheric muon flux in AMANDA-II MC-data deviation: ~ 7.5% There is a systematic effect around 30 degrees from vertical Horizontal resolution is still poor

Other things to look at… Other ice models Different depths Different times of the year Energy threshold dependence Vertical depth intensity Comparisons with other groups

Acknowledgments Dr. Paolo Desiati Dr. Albrecht Karle The UW-Madison AMANDA group The AMANDA collaboration Dr. Bob Benjamin The astrophysics REU group National Science Foundation

Dependence on energy: MC, E = 50 GeV Data, E = 50 GeV MC, E = 25 GeV

AMANDA and Cherenkov light