XV SEA (2022) Poster Contribution. Moving groups and stellar associations are privileged astrophysical tools to calibrate evolutionary models and to estimate ages of their members, given their coevality. Age, however, can display disparate results depending on the method with which it is estimated. Most recent data releases have made possible to obtain detailed information of memberships and to study stellar flux variability through accurate photometric time series (lightcurves). This has enriched our comprehension of phenomena like stellar rotation, its relationship with stellar activity and evolution, and ultimately its use for age estimation in stellar associations (i.e., gyrochronology). This method, however, still lacks agreement on the fundamental processes driving the angular momentum loss throughout the early history of stars, for which several models with different physical foundations currently coexist, still implementing new calibrations and formulations while feeding from the ever-growing new rotation period data available. We present the results of our work to rotationally characterize the population of the open cluster M39, and to estimate its age by comparison with other clusters and by implementing two recent gyrochronology models. This cluster lies at approximately 300 pc, with the latest age estimates ranging between 280-380 Myr. We obtain an age of 350 Myr, coeval with NGC 3532.