Planets and planetesimals form ubiquitously in extra-Solar planetary systems and are built from circumstellar material, present as leftover dust and gas from star-formation. 
The formation of these large planet/planetesimal bodies occurs during two main phases. Either these form in gas-rich protoplanetary disks during the first few Myr of a star's life, or later, from rocky planetesimal collisions over 10s to 100s of Myr. Planetesimal collisions also form dusty debris disks, structures that can survive over Gyr timescales. In both cases, planet-disk interactions can shape the morphologies of disks and give rise to distinct disk sub-structures dependent on planetary architectures and system-wide evolutionary processes. JWST, ALMA and other high angular resolution instruments are now resolving the morphologies and sub-structures of disks, and are thus providing critical data to understand how and where planets form, and how planetary systems evolve over their complete life cycles. Nevertheless, a number of core open questions remain: which types of sub-structures are present in protoplanetary and mature debris disks, on what timescales do these evolve, and under what conditions are planets uniquely responsible for these sub-structures? In this talk, I will give an outline of the recent history and findings in this topic, present new results that highlight progress answering these questions, and discuss future trends to explore with upcoming observations and facilities.