sub-millimetric emission from planets and asteroids of the Solar system and with instrumental noise. [[*Planck*]{}’s ]{}frequency response and beam shapes are modelled conforming to the present knowledge of [[*Planck*]{}’s ]{}receivers and its optical system. In order to extract the SZ-cluster signal, filtering schemes based on matched and scale-adaptive filtering are extended to spherical data sets.

In contrast to the recent work by @2004astro.ph..6190G, our SZ-simulation does not rely on idealised scaling relations and futhermore, takes account of the cluster’s morphological variety. The Galactic foregrounds are modelled in concordance with WMAP observations [see @2003ApJS..148...97B], which constitues an improvement over the simplifying assumptions made by Geisb[ü]{}sch et al. In addition, instrumentation issues such as non-isotropic detector noise are properly incorporated into the simulation. The filter scheme employed in the paper by Geisb[ü]{}sch et al. is the harmonic-space maximum entropy method introduced by @2002MNRAS.336...97S which assumes approximate prior knowledge of the emission component’s power spectra. Its computational demand is much higher than matched and scale-adaptive filtering: In fact, the computations presented in this work can be run on a notebook-class computer.

The paper is structured as follows: After a brief recapitulation of the SZ-effect in Sect. \[sect\_szdef\], the [[*Planck*]{}]{}-satellite and instrumental issues connected 