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We describe a new method that allows us to quantitatively characterizegalactic satellites from analysis of disturbances in outer gas disks, withoutrequiring knowledge of their optical light. We have demonstrated the validityof this method, which we call Tidal Analysis, by applying it to local spiralswith known optical companions, including M51 and NGC 1512. These galaxies spanthe range from having a low mass companion (~ one-hundredth the mass of theprimary galaxy) to a fairly massive companion (~ one-third the mass of theprimary galaxy). This approach has broad implications for many areas ofastrophysics - for the indirect detection of dark matter (or dark-matterdominated dwarf galaxies), and for galaxy evolution in its use as a decipher ofthe dynamical impact of satellites on galactic disks. Here, we present somepreliminary results on the emergent SEDs and images, calculated along the timesequence of these dynamical simulations using the 3-D self-consistent MonteCarlo radiative transfer code RADISHE. We explore star formation prescriptionsand how they affect the emergent SEDs and images. Our goal is to identify SEDcolors that are primarily affected by the galaxy's interaction history, and notsignificantly affected by the choice of star formation prescription. Ifsuccessful, we may be able to utilize the emergent UV-IR SED of the primarygalaxy to understand its recent interaction history.

Spikes in the SED and Ripples in the Outskirts of Galaxies