Lepton/neutrino/hadronic shower flux conversion

This script converts between a neutrino flux, a neutrino to lepton conversion rate, a muon flux or a hadronic shower flux to a neutralino annihilation rate or to a scattering cross section. This script calls the program flxconv written by Joakim Edsjö. If you use these results, the proper way to refer to them is to refer to this page and the publication M. Blennow, J. Edsjö and T. Ohlsson, JCAP 01 (2008) 021. [arXiv: 0709.3898] and to the program package WimpSim, WIMP annihilation Monte Carlo, J. Edsjö, www.fysik.su.se/~edsjo/wimpsim. In the publication above and in the documentation with the WimpSim Monte Carlo, you will also find more details about how these conversion factors are calculated.

NOTE 1. Compared to earlier versions of this script, this new script contains many more options. Please read them through carefully so that you understand what they mean. They are based on WimpSim runs of 10 000 000 annihilation events per mass and annihilation channel including best-fit neutrino oscillation parameters. The detector chosen (only affects the neutrino propagation through the Earth for Sun WIMPs) is IceCube for the time of year where the Sun is below the horizon. The choice of detector location has very little significance of the resulting fluxes though and this script can safely be used also for other detectors.

NOTE 2. As of 2009-03-17, this script also contains the possibility to convert to/from spin-independent or spin-dependent scattering cross sections. If you use this option, please refer to G. Wikström and J. Edsjö, JCAP 04(2009)009, [arXiv: 0903.2986]. The conversions here follow the standard calculation as outlined in that publication (i.e. we assume that either the spin-independent or spin-dependent scattering cross section dominates and that we have equilibrium between capture and annihilation in the Sun/Earth).

NOTE 3. If you want to have the code behind this script, you can download it here. Just download it and compile and link to DarkSUSY.

NOTE 4. As of 2009-04-23, a Kaluza Klein (UED) dark matter annihilation mixture is availabe as an annihilation channel. This channel is the same as available in WimpSim. It assumes a top mass of 172.4 GeV and puts the branching fraction to t t-bar to zero below this mass.

NOTE 5. 2015-09-27: In late 2009, in WimpSim 2.12 a bug that afffected neutrinos undergoing multiple neutral current interactions was fixed. This means that heavy WIMPs (TeV scale) annihilating to hard channels in the Sun had too low fluxes prior to version 2.12. This was fixed in WimpSim 2.12 and new WimpSim tables where this is fixed were released in DarkSUSY 5.1. However, the script below still uses the old uncorrected data tables. I will update the script shortly, but meanwhile, please use the offline code linked to DarkSUSY 5.1 or later instead.

DISCLAIMER! This cgi-script is provided as it is. If you encounter any problems, let me know.


GENERAL SETTINGS

WIMP mass [GeV]:
Annihilation place:
Annihilation channel:
Target density (g/cm3):

STARTING FLUX (to convert from)

Flux kind:
Flux type:
Energy [GeV]:
Angle from source [degrees]:
Conversion rate / flux / cross section[km-3 yr-1 / km-2 yr-1 / s-1 / pb]:

ENDING FLUX (to convert to)

Flux kind:
Flux type:
Energy [GeV]:
Angle from source [degrees]:

Note: For scattering cross sections and the annihilation rate, the kind, energy and angle are neglected as they are not needed for the conversion.


Questions? Send Joakim Edsjö an e-mail.