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Despite the numerous theories developed over the last few decades, the fundamental question of why some galaxies are dominated by a spheroidal component while others exist largely as rotationally-supported disk systems remains unresolved. Is the difference a consequence of initial conditions, galaxy interactions, or internal evolution ? The complete answer is undoubtedly a complicated mixture of all three mechanisms. In this poster, we access the importance of environmentally-related processes. Broadband R and near infrared images to are used to determine the variation in bulge-to-disk ratios for galaxies which are members of groups displaying a range in galaxy number density and richness. These data thus allow us to determine if correlations exist between the local present-day environments and basic galactic structures. Using H$\alpha$ imaging, the ongoing star forming properties of the group members are compared. Finally, we take advantage of the 1-degree field of view of the H$\alpha$ images to investigate the line-emitting dwarf galaxy population within the different group environments to see if the nature of the group members is correlated with the presence or absence of dwarfs.
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