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 age of a star cannot be measured but only inferred from observational quantities related to age. For stars in the red-giant phase, classical methods such as isochrone fitting can deliver ages with statistical uncertainties between 30% and 50%. Asteroseismic modelling is known to provide the most precise ages for red giants to date. Furthermore

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