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Waves have long been thought to contribute to the heating of the solar coronaand the generation of the solar wind. Recent observations have demonstratedevidence of quasi-periodic longitudinal disturbances and ubiquitous transversewave propagation in many different coronal environments. This paperinvestigates signatures of different types of oscillatory behaviour, both abovethe solar limb and on-disk, by comparing findings from the CoronalMulti-channel Polarimeter (CoMP) and the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) for the same active region. We studyboth transverse and longitudinal motion by comparing and contrastingtime-distance images of parallel and perpendicular cuts along/across activeregion fan loops. Comparisons between parallel space-time features in CoMPDoppler velocity and transverse oscillations in AIA images are made, togetherwith space-time analysis of propagating quasi-periodic intensity features seennear the base of loops in AIA. Signatures of transverse motions are observedalong the same magnetic structure using CoMP Doppler velocity(Vphase=600-750km/s, P=3-6mins) and in AIA/SDO above the limb (P=3-8mins).Quasi-periodic intensity features (Vphase=100-200km/s, P=6-11mins) also travelalong the base of the same structure. On the disk, signatures of bothtransverse and longitudinal intensity features were observed by AIA; both showsimilar properties to signatures found along structures anchored in the sameactive region three days earlier above the limb. Correlated features arerecovered by space-time analysis of neighbouring tracks over perpendiculardistances of <2.6Mm.

First comparison of wave observations from CoMP and AIA/SDO