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 neutrino yield [cm^2 sec sr] in form of the table
by reasing out the pre-stored propagation matrix data
via the PropagationMatrixFactory.
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.
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.
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
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 handles the table containing
the atmospheric muon flux calculated by PropagatingAtmMuonFlux
class PropagatingAtmMuonFlux.getDFMuDLogE(logE,cosZenith)
for combinations of alpha and Eth in AtmMuonBundleFlux.
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 log differential Flux dF/dLogE [/cm^2 sec sr]
after the propagation in the universe (with taking into account
the neutrino oscillation)
input: logEnergy [GeV]
output: neutrino fluxes after neutrino oscillation
(0: nu_e, 1:nu_mu, 2:nu_tau)
Calculate the log differential Flux dF/dLogE [/cm^2 sec sr]
after the propagation in the universe (with taking into account
the neutrino oscillation)
Calculation is based on a paper of J.
Calculate dF^2/dLogEcrDLogE [/cm^2 sec sr] for nu-mu
Because the cosmic ray follows the rapidly falling spectrum, the flux is
averaged over a given log(cosmic ray energy [GeV]) in a half width given
by halfWidthOfLogE.
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.
Calculate the differential Energy Flux [GeV /cm^2 sec sr]
after the propagation in the universe (with taking into account
the neutrino oscillation)
input: logEnergy [GeV]
output: neutrino fluxes after neutrino oscillation
(0: nu_e, 1:nu_mu, 2:nu_tau)
Calculate the differential Energy Flux [GeV /cm^2 sec sr]
after the propagation in the universe (with taking into account
the neutrino oscillation)
input: logEnergy [GeV]
particleID
1 nu-e
2 nu-mu
3 nu-tau (No nu-tau in the GZK model)
Implementation 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)
Return the log(neutrino cross section [cm^2])
for a given log10(neutrino energy [GeV]) that yields
numEvents with log10(neutrino energy flux [GeV/cm^2 sec sr])
Make a map of (neutrino crosssection [cm^2],
log10(neutrino energy flux [GeV/cm^2 sec sr])) for a given
log10(neutrino energy [GeV]) and the number of events
Uses a SwingWorker to perform time-consuming tasks in JulietEventGenerator
such as generating the Interaction Matrix and running
the propagating particle.
This class implements the main method to run
PropagatingAtmMuonFlux.getDFMuDLogCREDLogE(logCRE, logMuonE, cosZenith),
dF^2/dLogEcrDlogEmu, to make the numerical table for IceCube
downstream analysis.
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.
Print the yield table the method readYieldTable reads out
in the constructor for a given log(Neutrino Energy [GeV])
This method is mainly for debugging purposes.
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.
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.
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.
It calculates the detectable neutrino event intensity
at the Earth Surface as I3ParticleFlux does
but the calculation is made by using
the calculated energy distribution by NeutrinoQuickPropagator class
and the numerically calculated effective area (I3EffectiveArea.java)
without relying on I3Particle MC events.
The muon bundle flux table relative to those given by
the original parameters (alpha=2.04 Eth=3730=GeV - settable by the constructor
in this class) to a given alpha with the fixed Eth.
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.
This class makes and handles histograms of
the neutrino detection yield[cm^2 sec sr] generated by
DumpQuickPropagationMatrixYield class
and neutrino cross section.