Turbulence within protoplanetary disks plays a crucial role in the formation and evolution of planets, through its influence on processes ranging from the collisional velocity of small dust grains to the ability of gas-giant planets to open gaps in the disk. Because of this importance, more observational constraints are needed. Molecular line observations provide the most direct method for measuring gas motion, and we now have the sensitivity and resolution needed to constrain turbulence. I will discuss recent detections of turbulence around DM Tau and IM Lup, recent efforts to expand this sample, as well as the prospects for measuring radial and vertical variations in the turbulence, in the hopes of understanding the physical mechanism driving turbulence.