Abstract: Transverse oscillations in coronal loops, interpreted as MHD kink modes, are a key seismological tool for probing the dynamics and energy transport in the solar corona. However, inferring the polarisation of these oscillations—critical for understanding their energy fluxes and heating potential—has traditionally required coordinated observations from multiple instruments. In this talk, I will present a novel approach using only one instrument: The Coronal Multi-channel Polarimeter (CoMP). With CoMP observations we can simultaneously track plane-of-sky motions and Doppler velocities, and construct a phase portrait of the oscillation. By combining these measurements with a Bayesian framework, we can infer the polarisation and constrain the true displacements and velocity amplitudes of the oscillations, providing new insights into their energy transport and deposition. This method not only simplifies the observational requirements but also opens the door to systematic studies of wave polarisation across a wide range of coronal structures. I will discuss the implications of our findings for coronal seismology, and the broader question of how wave energy contributes to coronal heating.