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 effectiveness of determining P_rot heavily depends on the length of the observation period. Previously, apart from the long observation campaigns of TESS, it was not possible to measure rotation periods longer than about 13 days, half of TESS's 27-day sector observation period. TESS has completed two all-sky observations; combining these multi-sector data allows us to probe rotation periods beyond the typical limit of around 13 days. Measuring the rotation period from combined multi-sector data is challenging due to intra-sector gaps (every ~13 days), sector gaps, and phase shifts in the light curve when combining data with large gaps. In this work, we evaluate the limits of going up to ~20 days from at least two continuous sectors in multiple campaigns, the minimum possible multi-sector/cycle configuration. We assess the best strategies to extract P_rot and provide yields based on Kepler data observed as TESS cycles.