Dust in Clusters of Galaxies
  The presence of dust in the intracluster medium (ICM) has been a
long-standing problem that is still awaiting elucidation. Direct observational
diagnostics are rather challenging (though not impossible) either because of a
sparse distribution of dust in the intracluster space that makes extinction
measurements difficult or because of a low surface brightness of infrared
emission from dust. Complex indirect approaches are currently available that
can overcome uncertainties and provide a reasonable understanding of the basic
regulations of the physical state of dust in the ICM. Contrary to the common
opinion that the hot ICM does not allow dust to survive and manifest, many
sparse observational data either directly point out that dust exists in the
intracluster space or its presence is consistent with the data. Highly
divergent data in direct evidence and highly uncertain indirect indicators are
often connected either with dust fragility in a hot environment, the possible
compactness of spatial (clumpy) dust distribution in the ICM, or dynamical
features of dust transport. The source of dust is obviously connected with
galaxies, and it turns out that in most cases, dust is carried from galaxies
into the ICM while being thermally and dynamically shielded against the hostile
influence of high-energy ions. In this review, we briefly discuss related
issues from observational and theoretical points of view, including the
transport of dust into the ICM, and the associated destructive and protective
mechanisms and their characteristic time scales.
