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SNR G0.9+0.1 is a well known source in the direction of the Galactic Centercomposed by a Supernova Remnant (SNR) and a Pulsar Wind Nebula (PWN) in thecore. We investigate the potential of the future Cherenkov Telescope Array(CTA), simulating observations of SNR G0.9+0.1. We studied the spatial andspectral properties of this source and estimated the systematic errors of thesemeasurements. The source will be resolved if the VHE emission region is biggerthan $\sim0.65'$. It will also be possible to distinguish between differentspectral models and calculate the cut-off energy. The systematic errors aredominated by the IRF instrumental uncertainties, especially at low energies. Wecomputed the evolution of a young PWN inside a SNR using a one-zonetime-dependent leptonic model. We applied the model to the simulated CTA dataand found that it will be possible to accurately measure the cut-off energy ofthe $\gamma$-ray spectrum. Fitting of the multiwavelength spectrum will allowus to constrain also the magnetization of the PWN. Conversely, a pure power lawspectrum would rule out this model. Finally, we checked the impact of thespectral shape and the energy density of the Inter-Stellar Radiation Fields(ISRFs) on the estimate of the parameters of the PWN, finding that they are notsignificantly affected.

Constraining Models of the Pulsar Wind Nebula in SNR G0.9+0.1 via Simulation of its Detection Properties using the Cherenkov Telescope Array