  SNR G0.9+0.1 is a well known source in the direction of the Galactic Center
composed by a Supernova Remnant (SNR) and a Pulsar Wind Nebula (PWN) in the
core. We investigate the potential of the future Cherenkov Telescope Array
(CTA), simulating observations of SNR G0.9+0.1. We studied the spatial and
spectral properties of this source and estimated the systematic errors of these
measurements. The source will be resolved if the VHE emission region is bigger
than $\sim0.65'$. It will also be possible to distinguish between different
spectral models and calculate the cut-off energy. The systematic errors are
dominated by the IRF instrumental uncertainties, especially at low energies. We
computed the evolution of a young PWN inside a SNR using a one-zone
time-dependent leptonic model. We applied the model to the simulated CTA data
and found that it will be possible to accurately measure the cut-off energy of
the $\gamma$-ray spectrum. Fitting of the multiwavelength spectrum will allow
us to constrain also the magnetization of the PWN. Conversely, a pure power law
spectrum would rule out this model. Finally, we checked the impact of the
spectral 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 not
significantly affected.
