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, observational constraints are needed, although they have been limited in the past. Molecular line observations provide the most direct method for measuring gas motion, and ALMA has provided the sensitivity and resolution needed to constrain turbulence. We will present recent detections of turbulence around DM Tau and IM Lup, recent efforts to expand this sample, as well as discuss the the prospects for measuring radial and vertical variations in the turbulence using CO/13CO/C18O/N2H+/DCO+ emission.