Context : Waves have long been thought to contribute to the heating of the solar corona and the generation of the solar wind .
Recent observations have demonstrated evidence of quasi-periodic longitudinal disturbances and ubiquitous transverse wave propagation in many different coronal environments .

Aims : This paper investigates signatures of different types of oscillatory behaviour , both above the solar limb and on-disk , by comparing findings from the Coronal Multi-channel Polarimeter ( CoMP ) and the Atmospheric Imaging Assembly ( AIA ) on board the Solar Dynamics Observatory ( SDO ) for the same active region .

Methods : We study both transverse and longitudinal motion by comparing and contrasting time-distance images of parallel and perpendicular cuts along/across active region fan loops .
Comparisons between parallel space-time diagram features in CoMP Doppler velocity and transverse oscillations in AIA images are made , together with space-time analysis of propagating quasi-periodic intensity features seen near the base of loops in AIA .

Results : Signatures of transverse motions are observed along the same magnetic structure using CoMP Doppler velocity ( v _ { phase } = 600 \rightarrow 750 { km~ { } s } ^ { -1 } , P = 3 \rightarrow 6 mins ) and in AIA/SDO above the limb ( P = 3 \rightarrow 8 mins ) .
Quasi-periodic intensity features ( v _ { phase } = 100 \rightarrow 200 { km~ { } s } ^ { -1 } , P = 6 \rightarrow 11 mins ) also travel along the base of the same structure .
On the disk , signatures of both transverse and longitudinal intensity features were observed by AIA , and both show similar properties to signatures found along structures anchored in the same active region three days earlier above the limb .
Correlated features are recovered by space-time analysis of neighbouring tracks over perpendicular distances of \lesssim 2.6 Mm .

Conclusions :