IRAS data have been able to demonstrate the presence of dust in the
 ICM (Inter Cluster Medium) connected with a few dominant galaxies
 centered in cooling flows of X-ray emitting gas. The grains are
 predominantly heated by the bombardment of fast electrons. The
 FIR-emission from the grains therefore becomes a sensitive probe of
 the temperature and density of the hot gas. Because the grains are
 destroyed by sputtering on a short time scale (about 10E7 yr), the
 mere presence of dust calls for an explanation. In some cases
 (NGC4696) dust may have been accreted from outside, but in other
 cases (Hydra A) this seems unlikely. For Hydra A we have shown that
 mass-loss from evolved stars produces an insufficient amount of dust
 to explain the FIR luminosity. Instead we argue, that dust is produced
 in connection with star formation in the flow. The detection of FIR
 emission from dust in the ICM will provide important constraints for
 cooling flow models. Dedicated ISO observations of a sample of
 cooling flows will (1) learn us about the abundance of dust,
 (2) give some insight into grain properties (temperatures/sizes) in
 hot gas, (3) give information on densities and temperatures of the
 hot gas, (4) test our hypothesis of dust production in cooling flows,
 (5) maybe supply indirect evidence for low-mass star formation, and
 (6) show if FIR-emission from dust is a major coolant in cooling flows.

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