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Pulsar wind nebulae (PWNe) represent the largest class of sources thatupcoming {\gamma}-ray surveys will detect. Therefore, accurate modelling oftheir global emission properties is one of the most urgent problems inhigh-energy astrophysics. Correctly characterizing these dominant objects is aneeded step to allow {\gamma}-ray surveys to detect fainter sources,investigate the signatures of cosmic-ray propagation and estimate the diffuseemission in the Galaxy. In this paper we present an observationally motivatedconstruction of the Galactic PWNe population. We made use of a modifiedone-zone model to evolve for a long period of time the entire population. Themodel provides, for every source, at any age, a simplified description of thedynamical and spectral evolution. The long term effects of the reverberationphase on the spectral evolution are described, for the first time, based onphysically motivated prescriptions for the evolution of the nebular radiussupported by numerical studies. This effort tries to solve one of the mostcritical aspects of one-zone modeling, namely the typical overcompression ofthe nebula during the reverberation phase, resulting in a strong modificationof its spectral properties at all frequencies. We compare the emissionproperties of our synthetic Pulsar Wind Nebulae population with the mostupdated catalogues of TeV Galactic sources. We find that the firmly identifiedand candidate PWNe sum up to about 50% of the expected objects in this classabove threshold for detection. Finally, we estimate that CTA will increase thenumber of TeV detected PWNe by a factor$\geq3$.

Modeling the {\gamma}-ray Pulsar Wind Nebulae population in our Galaxy