PPPC 4 DM ID - A Poor Particle Physicist Cookbook for Dark Matter Indirect Detection

We provide ingredients and recipes for computing signals of TeV-scale Dark Matter annihilations and decays.

Data and Results from 1012.4515 [hep-ph] (and 1009.0224 [hep-ph]).

If you use the data provided on this site, please cite:
    M.Cirelli, G.Corcella, A.Hektor, G.Hütsi, M.Kadastik, P.Panci, M.Raidal, F.Sala, A.Strumia,
    "PPPC 4 DM ID: A Poor Particle Physicist Cookbook for Dark Matter Indirect Detection'',
    arXiv 1012.4515, JCAP 1103 (2011) 051.

If you use the 'Fluxes at production', please also cite:
   P. Ciafaloni, D. Comelli, A. Riotto, F. Sala, A. Strumia, A. Urbano,
   "Weak corrections are relevant for dark matter indirect detection'',
    arXiv 1009.0224, JCAP 1103 (2011) 019,
where the energy spectra have been computed including electroweak corrections.

This is Release 1.0 (December 2010). Log of changes here.
Fluxes at production:

Complete fluxes at production, including EW corrections as computed in 1009.0224:

Mathematica  functions: The file dlNdlxEW.m provides the spectra  Log10 [d N/d Log10 x ]. The notebook Sample.nb shows how to load and use it.
   
Numerical tables: Each table provides the spectra dN/d Log10x of stable SM particles (positrons, antiprotons...), normalized per one annihilation.
The columns are: [ mDM, Log10x , dN/d Log10x for 34 primary channels ].
The primary channels are:
DM DM -->eL+eL-, eR+eR-, e+e-, μL+μL-, μR+μR-, μ+μ-, τL+τL-, τR+τR-, qq, cc, bb, tt, WL+WL-, WT+WT-,W+W-, ZL+ZL-, ZT+ZT-, Z+Z-, gg, γγ, hmhhmh, νeνe, νμνμ, ντντ, VV → 4e, VV → 4μ, VV → 4τ.
The non-polarized fluxes are just obtained as the appropriate average of the Left and Right or Longitudinal and Transverse ones.
The channel into Higgs bosons is given for the following cases of Higgs mass: mh = 115, 135, 170, 200, 300, 400, 500 GeV.
  Positrons
  Antiprotons
  Gamma rays
  Electron Neutrinos
  Muon Neutrinos
  Tau Neutrinos
  Antideuterons
  all of the above All the 7 tables, in a single zipped file.


Fluxes at production without EW corrections (for comparison with previous calculations):
Mathematica  functions: The file dlNdlxPythia.m provides the spectra  Log10 [d N/d Log10 x ].
The notebook Sample.nb shows how to load and use it. 
   
Numerical tables: Same as above, but here the primary channels are the following 18:
DM DM --> e+e-, μ+μ-, τ+τ-, qq, cc, bb, tt, W+W-, ZZ, gg, γγ, hmhhmh.
  Positrons
  Antiprotons
  Gamma rays
  Electron Neutrinos
  Muon Neutrinos
  Tau Neutrinos
  Antideuterons
  all of the above All the 7 tables, in a single zipped file.

Propagation functions for electrons and positrons everywhere in the Galaxy:

Energy loss coefficient function b[E, r, z] for electrons and positrons in the Galaxy: Mathematica function b.m, refer to the notebook Sample.nb for usage.
Annihilation
Positrons: The file ElectronHaloFunctGalaxyAnn.m provides the halo functions I(x,Es,r,z) at a point (r,z) in the Galaxy.
The notebook Sample.nb shows how to load and use it.
Decay
Positrons: The file ElectronHaloFunctGalaxyDec.m provides the halo functions I(x,Es,r,z) at a point (r,z) in the Galaxy
The notebook Sample.nb shows how to load and use it.

Propagation functions for charged cosmic rays at the location of the Earth:

Annihilation
Positrons: The file ElectronHaloFunctEarthAnn.m provides the halo functions I(x,Es,rEarth) at the location of the Earth.
The notebook Sample.nb shows how to load and use it.


  Table of fit coefficients for the reduced halo function I(λ)
(in the approximated formalism - see paper).


Antiprotons:
 Table of fit coefficients for the propagation function R(T).


Antideuterons:
 Table of fit coefficients for the propagation function R(T).
Decay
Positrons: The file ElectronHaloFunctEarthDec.m provides the halo functions I(x,Es,rEarth) at the location of the Earth.
The notebook Sample.nb shows how to load and use it.


  Table of fit coefficients for the reduced halo function I(λ)
(in the approximated formalism - see paper).


Antiprotons: Table of fit coefficients for the propagation function R(T).


Antideuterons: Table of fit coefficients for the propagation function R(T).

Fluxes of charged cosmic rays at the Earth, after propagation:

Annihilation
Positrons:
 Mathematica function: the file ElectronFluxAnn.m provides the spectra Log10 [d Φ/d Log10 E ].
Refer to the notebook Sample.nb for usage.


  Numerical table: provides the spectra dΦ/d Log10E.
The columns are: [ mDM, halo, propagation, Log10E , dΦ/d Log10E for 34 primary channels ].
The spectra are computed at a benchmark annihilation cross of <σv> = 10-26 cm3/s and renormalized multiplying by (mDM/GeV)2.
Units are particles/(cm2 s sr).
   
Antiprotons:
 Mathematica function: the file ProtonFluxAnn.m provides the spectra Log10 [d Φ/d Log10 K ].
Refer to the notebook Sample.nb for usage.


 
 Numerical table: provides the spectra dΦ/d Log10K.
The columns are: [ mDM, halo, propagation, Log10K , dΦ/d Log10K for 34 primary channels ].
The spectra are computed at a benchmark annihilation cross of <σv> = 10-26 cm3/s and renormalized multiplying by (mDM/GeV)2.
Units are particles/(m2 s sr).
   
Antideuterons:
 Mathematica function: the file DeuteronFluxAnn.m provides the spectra Log10 [d Φ/d Log10 (Kd/n) ].
Refer to the notebook Sample.nb for usage.


 
 Numerical table: provides the spectra dΦ/d Log10(Kd/n).
The columns are: [ mDM, halo, propagation, Log10(Kd/n) , dΦ/d Log10(Kd/n) for 34 primary channels ].
The spectra are computed at a benchmark annihilation cross of <σv> = 10-26 cm3/s and renormalized multiplying by (mDM/GeV)2.
Units are particles/(m2 s sr).
Decay
Positrons: Mathematica function: the file ElectronFluxDec.m provides the spectra Log10 [d Φ/d Log10 E ].
Refer to the notebook Sample.nb for usage.


  Numerical table: provides the spectra dΦ/d Log10E.
The columns are: [ mDM, halo, propagation, Log10E , dΦ/d Log10E for 34 primary channels ].
The spectra are computed at a benchmark decay life of τ = 1026 s and renormalized multiplying by (mDM/GeV).
Units are particles/(cm2 s sr). 
   
Antiprotons:
 Mathematica function: the file ProtonFluxDec.m provides the spectra Log10 [d Φ/d Log10 K ].
Refer to the notebook Sample.nb for usage.


 
 Numerical table: provides the spectra dΦ/d Log10K.
The columns are: [ mDM, halo, propagation, Log10K , dΦ/d Log10K for 34 primary channels ].
The spectra are computed at a benchmark decay life of τ = 1026 s and renormalized multiplying by (mDM/GeV).
Units are particles/(m2 s sr).
   
Antideuterons:
 Mathematica function: the file DeuteronFluxDec.m provides the spectra Log10 [d Φ/d Log10 (Kd/n) ].
Refer to the notebook Sample.nb for usage.


 
 Numerical table: provides the spectra dΦ/d Log10(Kd/n).
The columns are: [ mDM, halo, propagation, Log10(Kd/n) , dΦ/d Log10(Kd/n) for 34 primary channels ].
The spectra are computed at a benchmark decay life of τ = 1026 s and renormalized multiplying by (mDM/GeV).
Units are particles/(m2 s sr).

J factors for prompt gamma rays:
 
Annihilation
Mathematica function: the file JAnn.m provides Log10 [J(θ)].
Refer to the notebook Sample.nb for usage.
Decay
Mathematica function: the file JDec.m provides Log10 [J(θ)].
Refer to the notebook Sample.nb for usage.

Fluxes of Inverse Compton gamma rays:

Annihilation
Mathematica function: the file IICAnn.m provides the Inverse Compton halo functions  IIC(Eγ,Es,b,l).
Refer to the notebook Sample.nb for usage.

Such notebook contains also a Mathematica code bite to compute the resulting IC flux.
Decay
Mathematica function: the file IICDec.m provides the Inverse Compton halo functions  IIC(Eγ,Es,b,l).
Refer to the notebook Sample.nb for usage.

Such notebook contains also a Mathematica code bite to compute the resulting IC flux.

Fluxes of extragalactic gamma rays:
Cosmological Boost factor B: Mathematica function BoostF.m, refer to the notebook Sample.nb for usage.
Optical Depth of the Universe: transparency factor Exp[-τ ] for gamma rays: Mathematica function OpticalDepth.m, refer to the notebook Sample.nb for usage.
Annihilation
Mathematica function: the file EGgammaFluxAnn.m provides the spectra Log10 [d Φ/d Log10 E ].
Refer to the notebook Sample.nb for usage.
Decay
Mathematica function: the file EGgammaFluxDec.m provides the spectra Log10 [d Φ/d Log10 E ].
Refer to the notebook Sample.nb for usage.


Log of changes and releases:

[30 oct 2011] Fixed typo in Sample.nb about the units of the spectra of positrons (the units are particles/(cm^2 sec sr), not particles/(m^2 sec sr)). No new Release.
[30 oct 2011] Fixed bug in the labelling of the files 'JAnn.m' and 'JDec.m' (which was causing runaway loops when evaluated for some profiles). No new Release.


Contact: marco.cirelli@cea.fr .


Last updated: 30 october 2011