iceCube.uhe.neutrinoModel

Class NeutrinoFlux

java.lang.Object

iceCube.uhe.neutrinoModel.NeutrinoFlux

All Implemented Interfaces:

Function

public class NeutrinoFlux
extends java.lang.Object
implements Function

UHE Neutrino fluxes based on the following moels
are calculated from the table.

Extremely High Energy Neutrinos and their Detection
S.Yoshida et al.,

The Astrophysical Journal 479 547-559 (1997)


Extremely High Energy Neutrinos, Neutrino Hot Dark Matter, and the Highest Energy Cosmic Rays
S.Yoshida, G. Sigl and S. Lee,

Phys.Rev.Lett. 81 5505 (1998)


Probing grand unified theories with cosmic-ray, gamma-ray, and neutrino astrophysics
G.Sigl et al ,

Phys.Rev.Rev. D 59 043504 (1998)


Ultrahigh-energy Neutrino Fluxes and Their Constraints
O.E..Kalahsev, G. Sigl et al ,

Phys.Rev.Rev. D 66 063004 (2002)


GZK neutrinos after the Fermi-LAT diffuse photon flux measurment
M.Ahlers et al ,

Astropart. Phys. 34 106-115 (2010)


Cosmogenic neutrinos: parameter space and detectability from PeV to ZeV
K. Kotera, D.Allard, A.V.Olinto

JCAP 10 013 (2010)


Diffuse neutrino intensity from the inner jets of active galactic nuclei: Impacts of external photon fields and the blazar
Kohta Murase, Yoshiyuki Inoue, and Charles D. Dermer

Phys Rev D 90 023007 (2014)


Testing the newborn pulsar origin of ultrahigh energy cosmic rays with EeV neutrinos
Ke Fang, Kumiko Kotera, Kohta Murase, and Angela V. Olinto

Phys Rev D 90 103005 (2014)

Note that NO NEUTRINO OSCILATION was considered in these models.
One can access the original flux with getEFlux and/or getDFDLogE method.

The flux at the earth surface after propagation in space with neutrino
oscillation effect are also calculated based on the recent result of
the oscillation parameters.
One can access the flux after having the oscillation effect with getEFluxwzOsci
and/or getDFDLogEwzOsci.

The tables to contain the flux data is stored in $JAVADIR/classes/icecube/uhe/neutrinoModel
which are read out by this class.

Usage:
NeutrinoFlux  model-parameter

model-parameter 
                1  the GZK neutrinos m=0 Zmax = 2
                2  the GZK neutrinos m=2 Zmax = 2
                3  the GZK neutrinos m=2 Zmax = 4
                4  the GZK neutrinos m=4 Zmax = 4
                5  the GZK neutrinos m=4 Zmax = 5 gamma=1.5
                6  the GZK neutrinos m=7 Zmax = 5 gamma=1.5
                7  the Z-burst
                8  the Top Down (SUSY)
                9  the Top Down (QCD)
                10 the GZK neutrinos (by Sigl) m=3 Zmax=2 gamma=1 Emax=100ZeV
                11 the GZK neutrinos (by Sigl) m=5 Zmax=3 gamma=2 Emax=10ZeV
                12 the GZK neutrinos (by Ahles, Francis et al) Emin 10EeV best fit with the Fermi constraint
                   m=4.6 Zmax=2 gamma=2.5 Emax = 1ZeV
                13 the GZK neutrinos (by Ahles, Francis et al) Emax 10EeV max fit with the Fermi constraint
                   m=4.4 Zmax=2 gamma=2.1 Emax = 1ZeV
                14 the GZK neutrinos (by Ahles, Francis et al) Emax 10EeV min fit with the Fermi constraint
                   m=2.0 Zmax=2 gamma=2.88 Emax = 1ZeV
                15 the GZK neutrinos (by Kotera) Uniform, Emax 316 EeV
                16 the GZK neutrinos (by Kotera) SFR1, Emax 316 EeV
                17 the GZK neutrinos (by Kotera) GRB1, Emax 316 EeV
                18 the GZK neutrinos (by Kotera) FR2, Emax 316 EeV
                19 the GZK neutrinos (by Ahles, Francis et al) Emin 3EeV max fit with the Fermi constraint
                   m=5.35 Zmax=2 gamma=2.28 Emax = 1ZeV
                20 the GZK neutrinos (by Ahles, Francis et al) Emin 3EeV min fit with the Fermi constraint
                   m=2.0 Zmax=2 gamma=2.63 Emax = 1ZeV
                21 the GZK neutrinos (by Ahles, Francis et al) Emin 3EeV best fit with the Fermi constraint
                   m=4.05 Zmax=2 gamma=2.47 Emax = 1ZeV

                22 the GZK neutrinos (by Kotera) no evolution, CMB only, Emax 316 EeV
                23 the GZK neutrinos (by Ahles, Francis et al) maximal with the Fermi constraint
                                                m=7 Zmax=4 gamma=2.0 Emax=3ZeV
                24 The baseline E-2 flux - J(E)E^2 = 10^-8 [GeV/cm^2 sec sr] per neutrino flavor.
                25 GZK by simProp (Alosio et al) SFR, KneiskeEBL
                26 GZK by simProp (Alosio et al) SFR, SteckerEBL
                26 GZK by simProp (Alosio et al) SFR, CMB only
                28 GZK by simProp (Alosio et al) FR2, KneiskeEBL
                29 GZK by simProp (Alosio et al) FR2, SteckerEBL
                30 GZK by simProp (Alosio et al) FR2, CMB only
                31 AGN neutrinos (Murase et al) gamma = 2.0  CR loading factor 10
                32 AGN neutrinos (Murase et al) gamma = 2.3  CR loading factor 10
                33 Newborn pulsar neutrinos (Ke, Kumiko, Angela) SFR
                34 Newborn pulsar neutrinos (Ke, Kumiko, Angela) uniform
                35 AGN Blazars  (Padovani et al) HBL only Y_nu_gamma=0.8
                36 AGN Blazars  (Padovani et al) all Y_nu_gamma=0.8
                37 the GZK neutrinos (by Ahles, Francis et al) Emin 1EeV best fit with the Fermi constraint
                   m=3.2 Zmax=2 gamma=2.52 Emax = 1ZeV

particleID
                1  nu-e
                2  nu-mu
                3  nu-tau (No nu-tau in the GZK model) 

Constructor Summary

Constructors

Constructor and Description
NeutrinoFlux(int model) Constructor: Reads out from the table stored in iceCube/uhe/neutrinoModel logE [eV] dF/dE E^2 [eV/cm^2 sec sr].

Method Summary

Methods

Modifier and Type	Method and Description
double	getDFDLogE(double logEnergy, int particleID) calculate the log differential Flux dF/dLogE [/cm^2 sec sr] logEnergy [GeV] particleID 1 nu-e 2 nu-mu 3 nu-tau (No nu-tau in the GZK model)
double[]	getDFDLogEwzOsci(double logEnergy) 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)
double	getDFDLogEwzOsci(double logEnergy, int particleID) 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.
double	getEflux() Get the normalization E^2dF/dE [GeV/cm2 sec sr] for the power law model (model ID 24)
double	getEFlux(double logEnergy, int particleID) calculate the differential Energy Flux [GeV /cm^2 sec sr] logEnergy [GeV] particleID 1 nu-e 2 nu-mu 3 nu-tau (No nu-tau in the GZK model)
double[]	getEFluxwzOsci(double logEnergy) 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)
double	getEFluxwzOsci(double logEnergy, int particleID) 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)
double	getEnergyBase() Set the base energy [GeV] to define normalization E^2dF/dE [GeV/cm2 sec sr] for the power law model (model ID 24)
protected double[]	getFluxwzOsci(double logEnergy, double nueflux, double numuflux, double nutauflux) Calculate the neutrino flux at the earth surface after propgation in space with neutrino oscillation.
double	getFunction(int functionIndex, double[] parameters, double x) Interface to Integration class.
double	getLogEmax() Return the logEmax[GeV] setted for the power law model (model ID 24)
double	getPowerLawIndex() Get the powerlaw index for the power law model (model ID 24)
boolean	isPowerLaw() tell if the setted model is a powerlaw model or not
void	setEflux(double eFlux) Set the normalization E^2dF/dE [GeV/cm2 sec sr] for the power law model (model ID 24)
void	setEnergyBase(double eBase) Set the base energy [GeV] to define normalization E^2dF/dE [GeV/cm2 sec sr] for the power law model (model ID 24)
void	setLogEmax(double logEnergy) Set the logEmax[GeV] for the power law model (model ID 24)
void	setPowerLawIndex(double gamma) Set the powerlaw index for the power law model (model ID 24)

Methods inherited from class java.lang.Object

clone, equals, finalize, getClass, hashCode, notify, notifyAll, toString, wait, wait, wait

Constructor Detail

NeutrinoFlux

public NeutrinoFlux(int model)
             throws java.io.IOException

Constructor: Reads out from the table stored in iceCube/uhe/neutrinoModel logE [eV] dF/dE E^2 [eV/cm^2 sec sr]. Energy unit is transfered to GeV.

Throws:

java.io.IOException

Method Detail

setLogEmax

public void setLogEmax(double logEnergy)

Set the logEmax[GeV] for the power law model (model ID 24)

getLogEmax

public double getLogEmax()

Return the logEmax[GeV] setted for the power law model (model ID 24)

setEflux

public void setEflux(double eFlux)

Set the normalization E^2dF/dE [GeV/cm2 sec sr] for the power law model (model ID 24)

getEflux

public double getEflux()

Get the normalization E^2dF/dE [GeV/cm2 sec sr] for the power law model (model ID 24)

setPowerLawIndex

public void setPowerLawIndex(double gamma)

Set the powerlaw index for the power law model (model ID 24)

getPowerLawIndex

public double getPowerLawIndex()

Get the powerlaw index for the power law model (model ID 24)

isPowerLaw

public boolean isPowerLaw()

tell if the setted model is a powerlaw model or not

setEnergyBase

public void setEnergyBase(double eBase)

Set the base energy [GeV] to define normalization E^2dF/dE [GeV/cm2 sec sr] for the power law model (model ID 24)

getEnergyBase

public double getEnergyBase()

Set the base energy [GeV] to define normalization E^2dF/dE [GeV/cm2 sec sr] for the power law model (model ID 24)

getEFlux

public double getEFlux(double logEnergy,
              int particleID)

        calculate the differential Energy Flux [GeV /cm^2 sec sr] 

        logEnergy [GeV]

        particleID
                1  nu-e
                2  nu-mu
                3  nu-tau (No nu-tau in the GZK model)

getDFDLogE

public double getDFDLogE(double logEnergy,
                int particleID)

        calculate the log differential Flux dF/dLogE [/cm^2 sec sr] 

        logEnergy [GeV]

        particleID
                1  nu-e
                2  nu-mu
                3  nu-tau (No nu-tau in the GZK model)

getFluxwzOsci

protected double[] getFluxwzOsci(double logEnergy,
                     double nueflux,
                     double numuflux,
                     double nutauflux)

        Calculate the neutrino flux at the earth surface after propgation in space
        with neutrino oscillation.

        Calculation is based on a paper of J. Jones et al., PRD, 69, 033004 (2004)
        Note that the mixing between nu_e and nu_tau is known to be very small, so
        the mixing is ignored.

        input: logEnergy [GeV],
               nu_e flux before neutrino oscillation,
               nu_mu flux before neutrino oscillation,
               nu_tau flux before neutrino oscillation

        output: neutrino fluxes after neutrino oscillation 
                (0: nu_e, 1:nu_mu, 2:nu_tau)

getEFluxwzOsci

public double[] getEFluxwzOsci(double logEnergy)

        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)

getEFluxwzOsci

public double getEFluxwzOsci(double logEnergy,
                    int particleID)

        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)

getDFDLogEwzOsci

public double[] getDFDLogEwzOsci(double logEnergy)

        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)

getDFDLogEwzOsci

public double getDFDLogEwzOsci(double logEnergy,
                      int particleID)

        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. Jones et al., PRD, 69, 033004 (2004)
        Note that the mixing between nu_e and nu_tau is known to be very small, so
        the mixing is ignored.

        input: logEnergy [GeV]

        particleID
                1  nu-e
                2  nu-mu
                3  nu-tau (No nu-tau in the GZK model)

getFunction

public double getFunction(int functionIndex,
                 double[] parameters,
                 double x)

Interface to Integration class. This is for calculating the integfral flux. function index 0 : dF/dLogE before the neutrino oscillation function index 1 : dF/dLogE taking into account the neutrino oscillation

Specified by:

getFunction in interface Function