We present simultaneous ground-based radial velocity (RV) measurements and space-based photometric measurements of the young and active K dwarf Epsilon Eridani. These measurements provide a data set for exploring methods of identifying and ultimately distinguishing stellar photospheric velocities from Keplerian motion. We compare three methods we have used in exploring this data set: Dalmatian, an MCMC spot modeling code that fits photometric and RV measurements simultaneously; the FF‧ method, which uses photometric measurements to predict the stellar activity signal in simultaneous RV measurements; and Hα analysis. We show that our Hα measurements are strongly correlated with the Microvariability and Oscillations of STars telescope (MOST) photometry, which led to a promising new method based solely on the spectroscopic observations. This new method, which we refer to as the HH‧ method, uses Hα measurements as input into the FF‧ model. While the Dalmatian spot modeling analysis and the FF‧ method with MOST space-based photometry are currently more robust, the HH‧ method only makes use of one of the thousands of stellar lines in the visible spectrum. By leveraging additional spectral activity indicators, we believe the HH‧ method may prove quite useful in disentangling stellar signals.