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We have constructed and calibrated a spherically-symmetric,spatially-dependent particle transport and emission code for young pulsar windnebulae (PWNe). This code predicts the spectral energy distribution (SED) ofthe radiation spectrum at different positions in a PWN, thus yielding thesurface brightness vs. radius and hence the nebular size as function of energy.It also predicts the X-ray spectral index at different radii from the centralpulsar, depending on the nebular B-field profile and particle transportproperties. We apply the code to PWN G0.9+0.1 and fit these three functionsconcurrently, thus maximizing the constraining power of the data. We use aMarkov-chain-Monte-Carlo (MCMC) method to find best-fit parameters withaccompanying errors. This approach should allow us to better probe the spatialbehaviour of the bulk-particle motion, the $B$-field and diffusion coefficient,and break degeneracies between different model parameters. Our model willcontribute to interpreting results by the future Cherenkov Telescope Array(CTA) that will yield many more discoveries plus morphological details ofvery-high-energy Galactic PWNe.

Simultaneous Fitting of the Spectral Energy Density, Energy-dependent  Size, and X-ray Spectral Index vs. Radius of The Young Pulsar Wind Nebula PWN  G0.9+0.1