ICRC 2003 in Tsukuba. Testing the HiRes Detector Simulation against UHECR Data. Andreas Zech ( Rutgers University) for the HiRes - Fly´s Eye Collaboration. J.A. Bellido, R.W. Clay, B.R. Dawson, K.M. Simpson University of Adelaide
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( Rutgers University)
for the HiRes - Fly´s Eye Collaboration
University of Adelaide
J. Boyer, S. Benzvi, B. Connolly, C. Finley, B. Knapp, E.J. Mannel, A. O’Neil, M. Seman, S. Westerhoff
J. Belz, M. Munro, M. Schindel
Montana State University
G. Martin, J.A.J. Matthews, M. Roberts
University of New Mexico
D. Bergman, L. Perera,
S. Schnetzer, G.B. Thomson, A. Zech
N. Manago, M. Sasaki
University of Tokyo
T. Abu-Zayyad, J. Albretson, G. Archbold,
J. Balling, K. Belov, Z. Cao, M. Dalton,
A. Everett, J. Girard, R. Gray, W. Hanlon, P. Hüntemeyer, C.C.H. Jui, D. Kieda, K. Kim, E.C. Loh, K. Martens, J.N. Matthews, A. McAllister, J. Meyer, S.A. Moore, P. Morrison, J.R. Mumford, K. Reil,R. Riehle, P. Shen, J. Smith, P. Sokolsky, R.W. Springer, J. Steck, B.T. Stokes, S.B. Thomas, T.D. Vanderveen, L. Wiencke
University of Utah
J. Amann, C. Hoffman, M. Holzscheiter, L. Marek, C. Painter, J. Sarracino, G. Sinnis, N. Thompson, D. Tupa
Los Alamos National LaboratoryHiRes Collaboration
We need M.C. to calculate the acceptance of our
detectors for the flux measurement:
M.C. is also a powerful tool for resolution studies
and for tests of our reconstruction programs.
This requires a simulation program that
describes the shower development and
detector response as realistically as possible.
We want our code to simulate events under the exact data-taking conditions.The Role of Monte Carlo Simulations in the HiRes Experiment
The composition is
chosen from our HiRes
Stereo and HiRes/MIA
The Fly’s Eye Stereo
spectrum is used as an
input for the M.C.M.C. Input Energy & Composition
Gaisser-Hillas fit to the shower profile:
Fit parameters scale with primary energy:CORSIKA Shower Library (proton & iron)
(low amplitude) can
be measured from the
width of the FADC
Additional sky noise
is added to the M.C. to
get agreement with
data of a certain period.Adding Noise to the M.C.
FADC counts in all trigger channels
total noise tubes distribution
or:Testing how well we understand our experiment ...
Energy rescaled by - 6 %
Number of signal tubes
Error in Psi angle
Good weather conditions
Time tangent fit Chi Squared
Profile fit Chi Squared
Čerenkov light fraction
The Longitudinal Profile
calculated in the M.C.
is in good agreement
with results from CORSIKA.
- we fit CORSIKA density profiles to the sum of 3 exponentials.
- fits are parametrized with zenith angle and distance between detector and Xmax.Čerenkov Light Simulation
black: CORSIKA long. Čerenkov profile vs.
red: our M.C. simulation
red: CORSIKA lateral Čerenkov density vs.
radial distance in meter
black: our fit using the sum of 3 exp.