TESS serves as a formidable tool for investigating stellar variability. Nonetheless, the adaptation of methodologies employed in other space missions, such as Kepler, to deduce long stellar rotation periods or solar-like stellar pulsations has been a challenge. The advent of multiple sectors of data for most stars every two years with the extended

The evolution of surface magnetic features on stars, such as spots and faculae, produces modulations in light curves. These modulations allow us to measure the surface rotation period, P_rot, of stars from the main sequence (e.g., McQuillan et al. 2014; Santos et al. 2019, 2021) to the red-giant (Ceillier et al. 2017) phase. Nevertheless, the

Gyrochronology can yield useful ages for field main-sequence stars, a regime where other techniques are problematic. Typically, gyrochronology relations are calibrated using young (2 Gyr) clusters, but the constraints at older ages are scarce, making them potentially inaccurate and imprecise. In order to test the performance of existing relations