We investigate the nature of sustained kink oscillations in coronal loops, by looking at their properties and potential drivers in multiple observational datasets, including both imagers and spectrographs. Kink oscillations have been observed for many years in SDO/AIA, where a majority of them has been seen to dissipate quickly and to be associated with impulsive heating events (as during e.g. magnetic reconnection events). That until recently, when long-lived (decayless) kink oscillations have started to be observed more frequently with the advent of the high-resolution EUV imager on board Solar Orbiter (SolO-EUI). Their sustainability shows significant potential for coronal heating but their energy source still remains to be identified. A scenario of coronal loops seen as self-oscillatory systems where their footpoints are excited by quasi-steady granular or super-granular flows has received positive support recently. We investigate further this scenario by combining typical coronal diagnostics with chromospheric diagnostics given by the Swedish 1-m Solar Telescope (SST). In this contribution I will show preliminary results and future perspectives to this work, which has been funded by the Research Council of Norway (grant 324523).