Calculate the neutrino yield [cm^2 sec sr] in form of the table
by reasing out the pre-stored propagation matrix data
via the PropagationMatrixFactory.
Calibrate Lepton Transfer matrix when inelasiticity is extremele small
such as tau's pair creation and calculation of
the differential cross section for z = 1- y ~ 1 could not avoid
numerical error.
Check Lepton Transfer matrix when inelasiticity is extremele small
such as tau's pair creation and calculation of
the differential cross section for z = 1- y ~ 1 could not avoid
numerical error.
Make a chi2-based statistical comparison between
the two MCs (one with E**-1, another with E**-2, for example) with the muon bundle flux
and the real data
Draw the total cross section and the energy loss("beta term") by reading
the pre-calculated and serialized IntertactionMatrix object stored in the file.
Draw the total cross section and the energy loss("beta term") by reading
the pre-calculated and serialized IntertactionMatrix object stored in the file.
Calculate the neutrino detection effective area [km^2 sr]
(neutrino interaction probability convoluted)
by running PropagationMatrixFlux with EffAreaTable class.
This class makes a 2D histogram of Energy correlations
like Muon In-ice Energy Vs Primary Cosmic Ray enegry
(obtained by AtmMuonBundleFlux.java in the MuonModel package)
or Muon In-ice Energy Vs Muon Surface Energy
(using PropagationMatrixFactory.java in the propahgation package)
Written by S.
This class calculates differential flux dF/dLogE [/cm^2 sec sr]
of atm muons as a function of emg/hadron cascade energy deposited
in the detector volume.
This class calculates differential flux dF/dLogE [/cm^2 sec sr]
of muons/taus as a function of emg/hadron cascade energy deposited
in the detector volume expected irom a given UHE neutrino model
such as GZK.
This class calculates differential flux dF/dLogE [/cm^2 sec sr]
of muons/taus as a function of emg/hadron cascade energy deposited
in the detector volume expected from a neutrino flux with monochromatic energy
E^2dF/dE = 10^-9 GeV/cm^2 sec sr.
Calculate the Neutrino flux at the surface
to give numberOfEvents, but the yield [cm^2 sec sr]
given in the argument is added up to calculate the flux.
Calculate the Neutrino flux at the surface
to give numberOfEvents, but the yield [cm^2 sec sr]
given in the argument is added up to calculate the flux.
Calculate the effective energy [GeV] of the parent cosmic ray
for a given IN-ICE energy of the EHE muon bundle and its zenith angle
at the IceCube depth.
Inplementation of interface numRecipes.Function
used for numerical integration of the probability
of (E_muon/E0)/ Bar(E_muon/E0) multiplied by CosmicRayFlux (Energy x R)
Uses a SwingWorker to perform time-consuming tasks in JulietEventGenerator
such as generating the Interaction Matrix and running
the propagating particle.
Calculate the in-ice effective area table
by running I3ParticleFlux.getInIceEffectiveArea(double logEnergy,
double cosZenith, int flavor, int doublet).
This is the abstract class to define the methods for both intereactions and decay
that determines the pathlength and produced energy with the Monte Carlo method.
This class calculates differential flux dF/dLogE [/cm^2 sec sr]
of muons/taus as a function of emg/hadron cascade energy deposited
in the detector volume expected from a neutrino flux with monochromatic energy
E^2dF/dE = 10^-9 GeV/cm^2 sec sr.
This class calculates differential flux dF/dLogE [/cm^2 sec sr]
of neutrinos and charged leptons after propagation in the earth
for a given model of primary cosmic neutrino production in the Universe.
This class calculates differential flux dF/dLogE [/cm^2 sec sr]
of neutrinos and charged leptons after propagation in the earth
for a given model of primary cosmic neutrino production in the Universe.
This class makes a 2D/1D histogram of Energy correlations
of In-ice Energy Vs Surface Energy
(using PropagationMatrixFactory.java in the propahgation package)
Written by S.
It calculates the detectable neutrino event intensity
at the Earth Surface as I3ParticleFlux does
but the calculation is made by using directly
the zenith angle binned propagation matrix
and the numerically calculated effective area (I3EffectiveArea.java)
without relying on I3Particle MC events.
Calculate the transfer matrix
This matrix should be a diagonal matrix with just "Sigma",
because all the incident energy is deposited as a hadronic cascade.
Store the propagation matrix calculated so far
to the store matrix which save energy distribution
of neutrinos and leptons propagating to the current
location.
This is the 3rd version of SwingWorker (also known as
SwingWorker 3), an abstract class that you subclass to
perform GUI-related work in a dedicated thread.