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[Licence| Download | New Version Template] aeks_v2_0.tar.gz(23853 Kbytes)
Manuscript Title: CLUMPY: Jeans analysis, γ-ray and ν fluxes from dark matter (sub-)structures
Authors: Vincent Bonnivard, Moritz Hütten, Emmanuel Nezri, Aldée Charbonnier, Céline Combet, David Maurin
Program title: CLUMPY
Catalogue identifier: AEKS_v2_0
Distribution format: tar.gz
Journal reference: Comput. Phys. Commun. 200(2016)336
Programming language: C/C++.
Computer: PC and Mac.
Operating system: UNIX(Linux), MacOS X.
RAM: Between 500MB and 1GB depending on the size of the requested skymap
Keywords: Dark matter, Indirect detection, Jeans analysis, γ-rays, ν.
Classification: 1.1, 1.7, 1.9.

External routines: CERN ROOT (http://root.cern.ch), GSL (http://www.gnu.org/software/gsl), cfitsio (http://heasarc.gsfc.nasa.gov/fitsio/fitsio.html), HEALPix C++ and F90 (http://healpix.sourceforge.net/index.php), GreAT (http://lpsc.in2p3.fr/great) (for MCMC analyses only), and Doxygen (http://www.doxygen.org) (optional)

Does the new version supersede the previous version?: Yes

Nature of problem:
Calculation of dark matter profile from kinematic data, γ-ray and ν signals from dark matter annihilation/decay.

Solution method:
Solve the integro-differential Jeans equation (optimised for speed) for several generic distributions (dark matter profile, light profile, velocity anisotropy). Integration of the DM density (squared) along a line of sight for generic dark matter haloes with substructures (spatial, mass, concentration distributions). Draw full skymaps of γ-ray and ν emission from dark matter structures, smoothed by an instrument PSF using HEALPix tools.

Reasons for new version:
Many more functionalities and options have been added to the code.

Summary of revisions:
Inclusion of the PPPC4DMID spectra for gamma-ray and neytrino fluxes; HEALPix pixelisation for skymaps and angular power spectrum; DM profile triaxiality enabled; More mass-concentration options; Multi-level substructure boost; Jeans analysis module to compute dark matter profiles for stellar kinematic data; Improved ROOT and FITS output.

The diffuse extragalactic contribution to the signal (and γ-ray attenuation) as well as secondary radiation from dark matter remain to be included in order to provide a comprehensive description of the expected signal.

Running time:
This is highly dependent of the user-defined choices of DM profiles, precision ε and integration angle αint:
  • ~ 1 hour for a full skymap (including substructures) with αint = 0.1° and ε = 0.01;
  • ~= 1 mn for a 5° x 5° skymap (including substructures) with αint = 0.1° and ε = 0.01;
  • ~ 5 mn for a typical Jeans/MCMC analysis (on a 'ultrafaint'-like dwarf spheroidal galaxy) using a constant anisotropy profile.