The experimental astrophysics team is part of both the HESS and AMS collaborations. It is therefore best suited for search strategies based on a precise measurement of the energy spectra of various cosmic rays like gamma rays (HESS and AMSg) as well as   charged  particle such as positrons, anti-protons and anti-deuterons (AMS).  As part of our project and with tight connections with the theorists on this project , the team is developing a cosmic ray spectrum generator [24] including: the annihilation cross section rates and products (based on MicrOMEGAs, Sloop and interface with Pythia), the dark matter profile models (in our Galaxy or spheroidal galaxies, clumpy structure), the propagation of charged particles (CRACand the detector performance and acceptance.  Armed with these tools we can perform various analyses considering the wealth of data that is, and will soon be, available for indirect detection. Among some of the first investigations, the team will first focus on HESS data analyses and interpretations. This concerns the centre of the galaxy, where a rather hard spectrum has already been observed (in the 100 GeV to few TeV range). Those galaxies which present a cuspy luminous matter profile are a source of interest for the indirect search of dark matter. The generator will also be used to perform  a grand scan "a la LEP" over different SUSY breaking scenarios and other theoretical model extensions (NMSSM, extra-dimensions,..). This scan will be used for the present data interpretation and to derive sensitivity domains with HESSII (access to lower energy range, above 50 GeV). Similarly, with this tool we will explore the complementarity between the ground telescopes and the space detector (GLAST, AMS).

A large part of the group has been involved in the construction of the electromagnetic calorimeter of the AMS-02 mission. This sub-detector is a key ingredient to separate the rare positrons from the proton background, as well as the anti-protons from the electron background and to identify gamma rays. Different MSSM configurations have been tested to estimate AMS sensitivity in the gamma and positron channels [24,28] and scenarios proposing clumpy structure in the galactic dark matter are being and will be further investigated. Further studies, will include the antiproton and anti-deuteron, in particular by handling the complete propagation issues. Then, in order to derive experimental sensitivities, we want to apply the same propagation models for both the background and signal. When all the ingredients will be included in the generator, we will combine the different channels (charged particles and gamma) and explore the complementarity for  SUSY scenarios, but also other theoretical model extensions. A critical and detailed global re-analysis of the supposed EGRET excess involving all members of the ToolsDmColl is also on the agenda.