In the last decade very-high-energy (VHE) astronomy has emerged as a new astronomical window, allowing for the study of the most extreme astrophysical processes in our Universe. The current generation of Cherenkov Telescopes H.E.S.S, MAGIC and VERITAS has revealed the presence of about two hundred of such VHE sources in the gamma-ray sky [1]. This is however just the tip of the iceberg, and the improved capabilities of the next generation of instruments, the Cherenkov Telescope Array (CTA) [2], is expected to increase this number by about one order of magnitude.Â
Among the VHE sources that CTA will be able to study in detail, Galactic sources are particularly interesting, as they offer the opportunity to deepen into the physics leading to the observed gamma-ray emission both from a spectral and a morphological perspective. The improved capabilities of CTA in sensitivity and angular resolution will allow a detailed characterization of the high-energy processes taking place in pulsars and pulsar wind nebulae (PWNe), Gamma-ray binaries (GBs), microquasars (MQs), Supernova Remnants (SNRs), Novae explosions or Galactic Stellar Clusters (GSCs).Â
In this Master Thesis project, we will study the VHE emission from Galactic sources as observed with CTA. The candidate will make use of dedicated simulation and analysis pipelines (Python-based) to retrieve the observation strategy and the array configuration required to constrain the timing, morphology, and spectral properties of these sources. Mastering these CTA pipelines will also provide the candidate with the needed expertise on the analysis of high-level scientific data on a given Galactic/Extragalactic VHE gamma-ray source that the observatory will deliver (open-source) in the next years.