Modelling rotation curves in planet forming disks

Rotation curves have long been used in galactic astronomy to infer the presence of dark matter. In protoplanetary discs, thanks to the high spatial and spectral resolution of ALMA, they provide a powerful tool to probe the dynamical mass, revealing key properties of both the central star and the surrounding disc. Recently, disc kinematics has gained significant interest, as it directly traces the disc structure, unveils planet-disc interactions, and tests the presence of hydrodynamical instabilities. exoALMA, an ALMA Large Program, is dedicated to characterizing the kinematics of planet-forming environments with unprecedented precision. In this talk, I will present my work within the exoALMA collaboration, focusing on modeling rotation curves to constrain fundamental properties such as disc mass, stellar mass, and scale radius. Understanding these quantities allows us to investigate disc composition, compare with thermochemical models, and assess the efficiency of angular momentum transport.