The next few years will be exciting ones for studying disk galaxy structure, with the advent of the first large spectroscopic surveys at optical and radio wavelengths that will resolve the kinematics of thousands of nearby systems. This talk will focus on exploiting those surveys to measure the physical structure of disk galaxies. I will begin by highlighting our current understanding of galaxy mass distributions in a cosmological context, and how the next generation of spectroscopic surveys will address important outstanding questions. I will then discuss the subtleties of interpreting line-of-sight velocity fields, and present a model-based approach to fitting them that probes the underlying physical structure of the disk more directly than the standard tilted-ring technique. To illustrate, I will describe automated kinematic fits using the publicly available code DiskFit that constrain the incidence of bar-like flows in dozens of CALIFA DR1 Halpha velocity fields and discuss the prospects for studying bar kinematics on a much larger scale with MaNGA. Finally, I will report on progress towards developing a pipeline to model the thousands of resolved HI detections that SKA pathfinder surveys will begin to deliver in the next year or two – and the power of combining resolved optical and HI velocity fields for probing dark and luminous matter in nearby galaxy disks.