and for that reason not included in our analysis.

Due to the planet’s being point sources, their fast movement and their diverse surface temperatures it is not feasible to produce a template and extrapolate the fluxes with a common emission law to [[*Planck*]{}]{}-frequencies. Instead, flux maps have been produced directly for each of the nine [[*Planck*]{}]{}-channels separately taking account of the planetary motion, the solution of the heat balance equation laid down above and the finite beam-width. The analogous holds for asteroids, that are covered by the next chapter.

Submillimetric emission from asteroids {#foreground_asteroids}
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Asteroids and minor bodies of the Solar system are easily observed by infrared satellites such as ISO and possibly by sub-millimetric observatories . An estimation by @2002NewA....7..483C shows that a large number of asteroids ($\sim 400$) should yield signals detectable by [[*Planck*]{}]{}. The orbital motion of all asteroids is fast enough to cause double detections at different positions in the sky separated by half a year due to [[*Planck*]{}’s ]{}scanning strategy. In contrast to planets, asteroids are not well restricted to the ecliptic plane and appear up to ecliptic latitudes of $\beta{\lower.5ex\hbox{{$\; \buildrel < \over \sim \;$}}}30\degr$.

The thermal emission properties of asteroids are well 