AWG - Marseille nov-2001 Aart Heijboer Contents reconstruction status muon effective area event rates for some diffuse sources

AWG - Marseille nov-2001 Aart Heijboer Reconstruction status update Last software meeting AartStrategy performing well error estimastes too small

AWG - Marseille nov-2001 Aart Heijboer PDF was refitted better fit near PDF maximum better description of tails include (some) electronics simulation (hit merging) t r = time residual - offset exponential below 2 ns

AWG - Marseille nov-2001 Aart 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  confidence intervals) are correct, it means that 68% of the events are closer to the true value than the error estimate. In that case, the following quantity pull  true error / error estimate is normally distributed around 0, with 

AWG - Marseille nov-2001 Aart Heijboer  fit = 1.09  fit = 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-2001 Aart Heijboer Muon effective area log(E ) AartStrategy (error<1 o ) AartStrategy after cut Classic3DStrategy (error<1 o ) effective area (km 2 )

AWG - Marseille nov-2001 Aart Heijboer Dependence on azimuth angle E  > TeV E  < TeV cos(zenith) azimuth cos(zenith) < 0.5 # events passing cuts Indication of phi-dependence at low energies.

AWG - Marseille nov-2001 Aart Heijboer  = 0  = -90  = 90  = -180/+180 Top view of detector and corresponding azimuth angles NB: future productions will use new detector files with correct orientation on the seabed d06_c00_s00.det (10 strings) d07_c00_s00.det (14 strings)

AWG - Marseille nov-2001 Aart Heijboer Neutrino effective area Rebinned to see (perhaps) phi-dependence, but not enough statistics in this production. ?

AWG - Marseille nov-2001 Aart Heijboer GRB Calcrate.exe "2e-4*E**-2" Calcrate.exe "4.9e4*E**-3.6" Calcrate.exe "(x 5 && x 7) *6e-4*E**-2" Calcrate.exe "(x 5&&x 6.5)*94.8*E**-3" calcrate input spectra E 2 *dN/dE (GeV -1 m -2 s -1 sr -1 ) log(neutrino energy/GeV) Event rates for some diffuse sources atmospheric WB-Bound MPR version of WB-Bound GRB model (Waxman)

AWG - Marseille nov-2001 Aart Heijboer Event rates for some diffuse sources but this is as a function of neutrino energy... we cannot measure that. next step: make this plot as function of (reconstructed) muon energy

AWG - Marseille nov-2001 Aart Heijboer

AWG - Marseille nov-2001 Aart Heijboer

AWG - Marseille nov-2001 Aart Heijboer