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The structure of magnetic fields in galaxies remains poorly constrained,despite the importance of magnetism in the evolution of galaxies. Radiosynchrotron and far-infrared dust polarization (FIR) polarimetric observationsare the best methods to measure galactic scale properties of magnetic fields ingalaxies beyond the Milky Way. We use synthetic polarimetric observations of asimulated galaxy to identify and quantify the regions, scales, and interstellarmedium (ISM) phases probed at FIR and radio wavelengths. Our studied suite ofmagnetohydrodynamical cosmological zoom-in simulations featureshigh-resolutions (10 pc full-cell size) and multiple magnetization models. Oursynthetic observations have a striking resemblance to those of observedgalaxies. We find that the total and polarized radio emission extends toapproximately double the altitude above the galactic disk (half-intensity diskthickness of $h_\text{I radio} \sim h_\text{PI radio} = 0.23 \pm 0.03$ kpc)relative to the FIR total and polarized emission that are concentrated in thedisk midplane ($h_\text{I FIR} \sim h_\text{PI FIR} = 0.11 \pm 0.01$ kpc).Radio emission traces magnetic fields at scales of $\gtrsim 300$ pc, whereasFIR emission probes magnetic fields at the smallest scales of our simulations.These scales are comparable to our spatial resolution and well below thespatial resolution ($<300$ pc) of existing FIR polarimetric measurements.Finally, we confirm that synchrotron emission traces a combination of the warmneutral and cold neutral gas phases, whereas FIR emission follows the densestgas in the cold neutral phase in the simulation. These results are independentof the ISM magnetic field strength. The complementarity we measure betweenradio and FIR wavelengths motivates future multiwavelength polarimetricobservations to advance our knowledge of extragalactic magnetism.

Extragalactic Magnetism with SOFIA (SALSA Legacy Program). VII. A  tomographic view of far infrared and radio polarimetric observations through  MHD simulations of galaxies