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State of the art radial velocity (RV) exoplanet searches are limited by theeffects of stellar magnetic activity. Magnetically active spots, plage, andnetwork regions each have different impacts on the observed spectral lines, andtherefore on the apparent stellar RV. Differentiating the relative coverage, orfilling factors, of these active regions is thus necessary to differentiatebetween activity-driven RV signatures and Doppler shifts due to planetaryorbits. In this work, we develop a technique to estimate feature-specificmagnetic filling factors on stellar targets using only spectroscopic andphotometric observations. We demonstrate linear and neural networkimplementations of our technique using observations from the solar telescope atHARPS-N, the HK Project at the Mt. Wilson Observatory, and the Total IrradianceMonitor onboard SORCE. We then compare the results of each technique to directobservations by the Solar Dynamics Observatory (SDO). Both implementationsyield filling factor estimates that are highly correlated with the observedvalues. Modeling the solar RVs using these filling factors reproduces theexpected contributions of the suppression of convective blueshift androtational imbalance due to brightness inhomogeneities. Both implementations ofthis technique reduce the overall activity-driven RMS RVs from 1.64 m/s to 1.02m/s, corresponding to a 1.28 m/s reduction in the RMS variation. The techniqueprovides an additional 0.41 m/s reduction in the RMS variation compared totraditional activity indicators.

Estimating Magnetic Filling Factors From Simultaneous Spectroscopy and Photometry: Disentangling Spots, Plage, and Network