  The formation of galaxies is significantly influenced by galactic winds,
possibly driven by cosmic rays due to their long cooling times and better
coupling to plasma compared to radiation. In this study, we compare the radio
observations of the edge-on galaxy NGC 4217 from the CHANG-ES collaboration
catalog with a mock observation of an isolated galaxy based on the arepo
simulation that adopts the state-of-the-art two-moment cosmic ray transport
treatment and multiphase interstellar medium model. We find significant
agreement between the simulated and observed images and spectroscopic data.
Specifically, we find that (i) while the radio flux is sensitive to the
magnitude of the magnetic field, the shapes of intensity profiles are only
weakly dependent on the normalization of the magnetic field and are robustly
predicted by our galaxy simulations; (ii) the multi-wavelength spectrum above
0.1~GHz is in agreement with the radio observations and its slope is also only
weakly sensitive to the magnetic field strength; (iii) the magnetic field
direction exhibits an X-shaped morphology, often seen in edge-on galaxies,
which is consistent with the observations and indicates the presence of a
galactic-scale outflow. Since the normalization of the intensity profiles and
spectrum are degenerate with respect to the magnetic field strength and the
normalization of the electron spectrum, this qualitative match is possible
provided that the simulated magnetic field is only mildly boosted, which could
be attributed to the missing galactic disk interaction with the CGM in our
idealized simulation. Our results highlight the importance of incorporating
advanced cosmic ray transport models in simulations and provide a deeper
understanding of galactic wind dynamics and its impact on galaxy evolution.
