  We present results obtained from our newly developed Galactic cosmic-ray
transport code PICARD, that solves the cosmic-ray transport equation. This code
allows for the computation of cosmic-ray spectra and the resulting gamma-ray
emission. Relying on contemporary numerical solvers allows for efficient
computation of models with deca-parsec resolution. PICARD can handle locally
anisotropic spatial diffusion acknowledging a full diffusion tensor. We used
this framework to investigate the transition from axisymmetric to spiral-arm
cosmic-ray source distributions. Wherever possible we compare model predictions
with constraining observables in cosmic-ray astrophysics.
