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We have simulated the Expanded Owens Valley Solar Array (EOVSA) radio imagesgenerated at multiple frequencies from a model solar active region, embedded ina realistic solar disk model, and explored the resulting datacube for differentspectral analysis schemes to evaluate the potential for realizing one ofEOVSA's most important scientific goals--coronal magnetography. In this paper,we focus on modeling the gyroresonance and free-free emission from an on-disksolar active region model with realistic complexities in electron density,temperature and magnetic field distribution. We compare the magnetic fieldparameters extrapolated from the image datacube along each line of sight afterfolding through the EOVSA instrumental profile with the original (unfolded)parameters used in the model. We find that even the most easily automated,image-based analysis approach (Level 0) provides reasonable quantitativeresults, although they are affected by systematic effects due to finitesampling in the Fourier (uv) plane. Finally, we note the potential for errorsdue to misidentified harmonics of the gyrofrequency, and discuss the prospectsfor applying a more sophisticated spectrally-based analysis scheme (Level 1) toresolve the issue in cases where improved uv coverage and spatial resolutionare available.

Coronal Magnetography of a Simulated Solar Active Region from Microwave Imaging Spectropolarimetry