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AWG - Marseille nov-2001Aart Heijboer
Contents reconstruction status muon effective area event rates for some diffuse sources
AWG - Marseille nov-2001Aart Heijboer
Reconstruction status update
Last month @ software meetingAartStrategy performing wellerror estimastes too small
AWG - Marseille nov-2001Aart Heijboer
PDF was refitted
better fit near PDF maximum better description of tails include (some) electronics simulation (hit merging)
tr = time residual - offset
exponential below 2 ns
AWG - Marseille nov-2001Aart Heijboer
intermezzo: pull distributions
ML estimators are, in the N ®¥ case, Normaly distributed (CLT) around the true value With a variance given by the Minimum Variance Bound
If the error estimates (1 s confidence intervals) arecorrect, it means that 68% of the events are closer tothe true value than the error estimate.
In that case, the following quantity pull º true error / error estimateis normally distributed around 0, with =1.s
AWG - Marseille nov-2001Aart Heijboer
sfit = 1.09
sfit = 1.10
pull now ok (too within 10%). This means Calculation method of error estimates understood Likelihood PDF correctly describes data Error estimates can be trusted!
AWG - Marseille nov-2001Aart Heijboer
Muon effective area
log(En)
AartStrategy (error<1o)AartStrategy after cutClassic3DStrategy (error<1o)
effective area (km2)
AWG - Marseille nov-2001Aart Heijboer
Dependence on azimuth angleEm > TeVEm < TeV
cos(
zenit
h)
cos(
zenit
h)
azimuth azimuth
azimuth azimuth
cos(zenith) < 0.5 cos(zenith) < 0.5
# events passing cuts# events passing cuts
# events passing cuts # events passing cuts
Indication of phi-dependence at low energies.
AWG - Marseille nov-2001Aart Heijboer
f = 0
f = -90 f = 90
f = -180/+180
Top view of detectorand corresponding azimuth angles
NB: future productions willuse new detector files with correctorientation on the seabedd06_c00_s00.det (10 strings)d07_c00_s00.det (14 strings)
AWG - Marseille nov-2001Aart Heijboer
Neutrino effective area
Rebinned to see (perhaps) phi-dependence, but not
enough statistics in this production.
?
AWG - Marseille nov-2001Aart Heijboer
GRB
Calcrate.exe "2e-4*E**-2"Calcrate.exe "4.9e4*E**-3.6"Calcrate.exe "(x<5)*2e-2*E**-2 + (x>5 && x<7)*126*E**-2.76 + (x>7) *6e-4*E**-2"Calcrate.exe "(x<5)*.3e-9*E**-1 + (x>5&&x<6.5)*3e-5*E**-2 + (x>6.5)*94.8*E**-3"
calcrate input spectra
E2*d
N/d
E (
GeV
-1 m
-2 s
-1 s
r-1)
log(neutrino energy/GeV)
Event rates for some diffuse sources
atmosphericWB-BoundMPR version of WB-BoundGRB model (Waxman)
AWG - Marseille nov-2001Aart Heijboer
Event rates for some diffuse sources
but this is as a function of neutrinoenergy... we cannot measure that.
next step: make this plot as function of (reconstructed) muon energy
AWG - Marseille nov-2001Aart Heijboer
AWG - Marseille nov-2001Aart Heijboer
AWG - Marseille nov-2001Aart Heijboer
