In this dissertation, I present a series of studies on the low surface brightness outskirts of galaxies, which contain a record of tidal interactions and secular evolution processes. Each study utilized new deep imaging from the Burrell Schmidt Telescope in either broadband filters or narrow-band filters targeting Halpha emission. Regarding tidal interactions, I present a study of the M96 Group (or Leo I Group), as well as deep imaging of the interacting pair M51. I find that the M96 Group’s intragroup light (IGL) consists of only three faint linear streams. I find no stellar counterpart to the group’s H I ring, unusual if it were collisional in origin, and few signs of interaction among its four most massive members, implying a very calm tidal history. In M51, I discover several extremely diffuse plumes of starlight, yet find no stellar counterpart to its H I tail. Additionally, I measure red (B - V ~ 0.8) colors in all of its most extended tidal features, implying dominantly old populations and thus a lack of interaction-induced extended star formation. Regarding secular evolution, I conduct a detailed photometric study of three nearby galaxies’ outer disks. Each outer disk lacks both ongoing star formation and the spiral structure necessary to migrate stars from the inner disk, hence it is unclear how these red outer disks formed. Finally, I conduct a study of the H II regions and diffuse ionized gas (DIG) throughout the M101 Group, to determine whether star formation in low density environments occupies a distinct physical regime from its high density counterpart. I find that the distribution of Halpha/FUV flux ratios (a tracer of the initial mass function, IMF) is constant among all H II region populations throughout the group. Also, the Halpha/FUV ratio in the DIG appears tied only to the local intensity of star formation, leaving little room for changing star formation physics. In total, this dissertation shows that tidal interactions in low-density groups may be infrequent, raises questions about the origin of extended red outer disks, and shows that star formation physics change little with local mass density.