to observation of CMB anisotropies are decribed in Sect. \[sect\_planck\]. The foreground emission components are introduced in Sect. \[sect\_foreground\]. The steps in the simulation of flux maps for the various [[*Planck*]{}]{}-channels are described and their correlation properties are examined in Sect. \[sect\_plancksim\]. The theory of matched and scale-adaptive filtering is extended to spherical data sets and the resulting filter kernel shapes are in detail discussed in Sect. \[sect\_filtering\]. A summary in Sect. \[sect\_summary\] concludes the paper.

Throughout the paper, the cosmological model assumed is the standard cosmology, which has recently been supported by observations of the WMAP satellite [@2003astro.ph..2209S]. Parameter values have been chosen as $\Omega_\mathrm{M} = 0.3$, $\Omega_\Lambda =0.7$, $H_0 = 100\,h\,\mbox{km~}\mbox{s}^{-1}\mbox{ Mpc}^{-1}$ with $h = 0.7$, $\Omega_\mathrm{B} = 0.04$, $n_\mathrm{s} =1$ and $\sigma_8=0.9$.

Sunyaev-Zel’dovich definitions {#sect_szdef}
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The Sunyaev-Zel’dovich effects are the most important extragalactic sources of secondary anisotropies in the CMB. Inverse Compton scattering of CMB photons with electrons of the ionised ICM gives rise to these effects and induce surface brightness fluctuations of the CMB sky, either because of the thermal motion of the ICM electrons (thermal SZ-effect) or because of the bulk motion of the cluster itself relative to the comoving CMB-frame along the line-of-sight 