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
define the geometry of propagating particles
double x_ice3 : x [cm] of a particle trajectory point in the IceCube coordinate
double y_ice3 : y [cm] of a particle trajectory point in the IceCube coordinate
double z_ice3 : z [cm] of a particle trajectory point in the IceCube coordinate
double nadirAngle_ice3 : nadir angle [deg] define in the IceCube coodrinate
double azimuthAngle_ice3 : nadir angle [deg] define in the IceCube coodrinate
define the geometry of propagating particles
double x_ice3 : x [cm] of a particle trajectory point in the IceCube coordinate
double y_ice3 : y [cm] of a particle trajectory point in the IceCube coordinate
double z_ice3 : z [cm] of a particle trajectory point in the IceCube coordinate
double nx,ny,nz : unit direction vector represented by the IceCube coordinate
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.
Options to calculate flux with/without taking into
account fluxcuation of muon energies due to
the EAS cascade process
true : Flux is calculated such that an event by event flucuation is included.
Get Cumulative Probability on a given log(Primary Energy [GeV]),
log(Produced Energy [GeV])
double logPrimaryEnergy : Log (Input Primary Energy [GeV])
double logPproducedEnergy : Log (Produced Energy [GeV] via this interaction)
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]
logEnergy [GeV] cos(zenith angle)
This method is indentical to getDFDLogE(double logEnergy)
because the cosmic ray flux is isotropic.
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]
logEnergy [GeV] cos(zenith angle)
This method is indentical to getEFlux(double logEnergy)
because the cosmic ray flux is isotropic.
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)
int functionIndex : 1 calculation with inice muon, 2 with the surface
double x = R = (E_muon/E0)/ Bar(E_muon/E0)
parameter[0] : log10(primary Cosmic Ray Energy [GeV]) to be responsible
for the muon bundle in AVERAGE i.e.
The Glashow Resonance reaction with W into the hadronic decay
\bar{nu_e} + e^{-1} -> hadrons
The super class GlashowResonanceLeptonic class is used
in most of the calculation
The inelasiticity parameter y is fixed to be always 0
because all the final states are hadrons that generates cascades at once.
Default Constructor
InputStream in : Stream to readout a series of I3Particles that is subject
to your analysis
It reads all I3Particles from InputStream and hold them in form
of List.
Constructor
InputStream in : Stream to readout a series of I3Particles that is subject
to your analysis
filterOutBadRunData : do not use events in the bad run.
Package icecube.uhe.muonModel
This package is essentially equivalent
to the neutrinoModel package but deals with
the atmospheric muon fluxes instead of primary
cosmic neutrino fluxes.
Package icecube.uhe.neutrinoModel
This package contains the classes to calculate
primary neutrino fluxes predicted in the EHE neutrino models
such as the GZK cosmogenic neutrino production.
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.
Matrix of the Energy Transfer by the mu decays
The matrix elements are calculated by the methods supplied
by the Decay class.
/------------------------------------------------------------\
logEmin | 0 0 ...................................
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.
Ported to Java by Shigeru Yoshida for the IceCube MC.
2002.12.1
syoshida@hepburn.s.chiba-u.ac.jp
Before using, initialize the state by the constrctor RandomDouble(long)
in this Java version.
Search the array index such that x is between xx[index]
and xx[index+1]. xx must be monotonic, either increasing
or decreasing. index =0 or index = n-1 is returned
to indicate x is out of range.
Set historgram bin size
double deltaLogEnergy bin size of logEnergy
double deltaLogNpe bin size of logNpe
double deltaCosZenith bin size of cos(zenith angle)
double deltaFgQuality bin size of "First Guess Quality index" in unit of beta
set all the GZK boundary values of Npe and cosZenith
in the "EHE Super Cut" for each of the four event categories:
Npe-ATWD > Npe-FADC && | Npe-ATWD < Npe-FADC &&
cobZ =[min max] | cobZ =[min max]
----------------------------------------------------
Npe-ATWD > Npe-FADC && | Npe-ATWD < Npe-FADC &&
cobZ out of [min max] | cobZ out of [min max]
The GZK boundary are defined by connecting the lines
from the i-th point to the i+1 th point.
set the mode on the flux caulation
boolean includeFluctuationEffects :
true default. calculate the flux taking into account flucuation of
muon energies due to the EAS cascading.
set the mode on the flux caulation
boolean includeFluctuationEffects :
true default. calculate the flux taking into account flucuation of
muon energies due to the EAS cascading.
Set range of MC primary spectrum dN/dE
double logEnergyMinimum : log(Energy Minimum [GeV]) in the spectral range
double logEnergyMaximum : log(Energy Maximum [GeV]) in the spectral range
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.
Matrix of the Energy Transfer by the tau decays
The matrix elements are calculated by the methods supplied
by the Decay class.
/------------------------------------------------------------\
logEmin | 0 0 ...................................