in microwave data.

In contrast, in the kinetic effect it is the peculiar motion of a cluster along the line of sight relative to the CMB frame that induces CMB surface brightness fluctuations. The peculiar motion of the cluster causes the CMB to be anisotropic in the cluster frame. Due to this symmetry breaking of the scattering geometry, photons scattered into the line-of-sight are shifted in frequency, namely to higher frequencies, if the cluster is moving towards the observer.

The [[*Planck*]{}]{}-mission will be especially suited to detect SZ-clusters due to its sensitivity, its spectroscopic capabilities, sky coverage and spatial resolution. It is expected to yield a cluster catalogue containing $\simeq10^4$ entries. Extensive literature exists on the topic, but so far the influence of foregrounds and details of [[*Planck*]{}’s ]{}instrumentation and data aquisition have not been thoroughly addressed. In this work we aim at modelling the astrophysical and instrumental issues connected to the observation of SZ-clusters as exhaustively as possible: A simulation is presented that combines realistic maps of both SZ-effects with a realisation of the CMB, with four different Galactic foreground components (thermal dust, free-free emission, synchrotron emission and emission from rotational transitions of CO molecules), with maps containing the 