We present a large-scale study of stellar rotation for T Tauri stars in the Orion star-forming complex. We use the projected rotational velocity (vsin(i)) estimations reported by the APOGEE-2 collaboration as well as individual masses and ages derived from the position of the stars in the HR diagram, considering Gaia-EDR3 parallaxes and photometry plus diverse evolutionary models. We find an empirical trend for vsin(i) decreasing with age for low-mass stars (0.4M_{sun}<M*<1.2M{sun}_). Our results support the existence of a mechanism linking vsin(i) to the presence of accreting protoplanetary disks, responsible for regulating stellar rotation on timescales of about 6Myr, which is the timescale in which most of the T Tauri stars lose their inner disk. Our results provide important constraints to models of rotation in the early phases of evolution of young stars and their disks.

Cone search capability for table J/ApJ/923/177/table1 (The Orion star-forming complex (OSFC) rotational velocities and rotational periods)

Cone search capability for table J/ApJ/923/177/table3 (Masses and ages for kinematic members with Teff<6500K)

Cone search capability for table J/ApJ/923/177/table4 (Rotational velocities and rotational periods for stars not included as kinematic or spectroscopic members)