We have used teraelectronvolt cosmic ray spectrum of electrons and positrons data from DArk Matter Particle Explorer (DAMPE) to estimate the upper limits on dark matter annihilation. We have created modeled spectrum of electrons and positrons by considering dark matter annihilation into electrons and positrons with different channels. After the production, electrons and positrons can lose their energy by interstellar medium and interstellar radiation field. We have considered loss processes such as inverse Compton scattering, synchrotron radiation and ionization. The upper limits on dark matter annihilation cross-section have been investigated by comparing the model spectrum and observational spectrum. The stringent constraints is from electron-positron channel.

Cosmic-ray electrons (and positrons) can be used to probe self-annihilation or decay of dark matter particles. We have used spectrum of high energy cosmic-ray electrons between 300 GeV and 5 TeV measured by Very Energetic Radiation Imaging Telescope Array System (VERITAS) to constrain dark matter annihilation cross-section in the solar neighbourhood. A diffusion-loss equation with a canonical model has been used as a spectrum model function by assuming a NFW profile for the Milky Way halo. We have considered cosmic-ray electrons as products of annihilation of heavy dark matter particles (GeV -TeV). During the propagation through interstellar medium, the cosmic-ray electrons lose their energy due to synchrotron radiation, inverse-Compton scattering and ionization processes.

Clusters of galaxies are the largest gravitationally-bound structures in the Universe. They are composed of galaxies and gas (approximately 15% of the total mass) mostly dark matter (DM, accounts up to 85% of the total mass). If the DM is composed of Weakly Interacting Massive Particles (WIMPs), galaxy clusters represent one of the best targets to search for gamma-ray signals induced by the decay of WIMPs, with masses around the TeV scale. Due to its sensitivity and energy range of operation (from 20 GeV to 300 TeV), the Cherenkov Telescope Array (CTA) Observatory has a unique opportunity to test WIMPs with masses close to the unitarity limit. This will complement the searches for DM from other gamma-ray observatories as well as direct and collider experiments. The CTA Observatory is planning to search for gamma-ray emission, either its origin may be cosmic-ray (CR) or DM related, in the Perseus galaxy cluster during the first years of operation. In this poster, we will present the software created to perform the analysis using the ctools software and the corresponding results.