clear. However for plume 3 there is some uncertainty due to the complicated superposition of probably several plumes along the line of sight. The radiance distribution around plume 3 in EUVI A is dominated by one prominent peak (marked as 3a in Figure \[fig:inten\_epi\_plot\]) with a smaller peak (3) on the right side, whereas in EUVI B two distinct peaks (3b and 3) appear. There are four possible ways to associate the two plume signatures in the two images. Trying all combinations, we judged their likelihood from the inclination of the resulting 3D plumes. When a point on the 3D plume leaves from its footpoint on the solar surface, its distance to the solar rotation axis should increase as well. The second criterion is that the angle between the plume and the local meridian plane passing through the plume footpoint should be as small as possible (see Figure \[fig:plume\_geometry\]). In this way, we find that the combination of peak 3 in image A and peak 3 in image B gave the most reasonable result. In Figure \[fig:cross\_sec\], we sketch the situation which we think yields the different peaks in the two images for plume 3. Here we assumed a circular 