We study the kinematical characteristics and 3D geometry of alarge-scale coronal wave that occurred in association with the 26April 2008 flare-CME event. The wave was observed with the EUVIinstruments aboard both STEREO spacecraft (STEREO-A and STEREO-B) witha mean speed of ~240 km s-1
. The wave is more pronounced in the easternpropagation direction, and is thus, better observable in STEREO-Bimages. From STEREO-B observations we derive two separate initiationcenters for the wave, and their locations fit with the coronal dimmingregions. Assuming a simple geometry of the wave we reconstruct its 3Dnature from combined STEREO-A and STEREO-B observations. We find thatthe wave structure is asymmetric with an inclination towards East. Theassociated CME has a deprojected speed of ~750±50 km s-1
, and shows anon-radial outward motion towards the East with respect to theunderlying source region location. Applying the forward fitting modeldeveloped by Thernisien, Howard, and Vourlidas (2006), we derive theCME flux rope position on the solar surface to be close to the dimmingregions. We conclude that the expanding flanks of the CME most likelydrive and shape the coronal wave.