In the process of star formation, the redistribution and removal of angular momentum play a fundamental role on scales ranging from the outer envelope to the disk, jet, and outflow. High-angular- and spectral-resolution observations, together with different theoretical models and numerical simulations, have characterized this transport from the outer envelope to the disk. The removal of excess angular momentum from the disk is essential, as it regulates the mass of the disk–protostar system, drives chemical changes in the surrounding material, and influences planet formation. Magnetocentrifugal mechanisms are thought to be the main processes responsible for this removal, whereby material is launched along vertical magnetic field lines anchored in the disk. These lines may be anchored in the innermost region of the disk, where the magnetosphere truncates it, giving rise to X-winds, or they may extend over a broader range of disk radii, giving rise to disk winds. Recent interferometric observations with the SMA and ALMA, together with infrared observations from JWST, have found evidence for disk winds in different protostellar systems. In this talk, I will discuss observations of the outflows from the protostellar systems CB 26, HH 212, HH 30, and HH 111, which have enabled the identification of kinematic components associated with disk winds. Combining these observations with theoretical models allows us to estimate their morphological and kinematic properties, as well as to investigate their interaction with X-winds.