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We study the infrared (IR) properties of galaxies in the cluster MS 1054-03at z=0.83 by combining MIPS 24 micron data with spectra of more than 400galaxies and a very deep K-band selected catalog. 19 IR cluster members areselected spectroscopically, and an additional 15 are selected by theirphotometric redshifts. We derive the IR luminosity function of the cluster andfind strong evolution compared to the similar-mass Coma cluster. The bestfitting Schechter function gives L*_{IR}=11.49 +0.30/-0.29 L_sun with a fixedfaint end slope, about one order of magnitude larger than that in Coma. Therate of evolution of the IR luminosity from Coma to MS 1054-03 is consistentwith that found in field galaxies, and it suggests that some internalmechanism, e.g., the consumption of the gas fuel, is responsible for thegeneral decline of the cosmic star formation rate (SFR) in differentenvironments. The mass-normalized integrated SFR within 0.5R_200 in MS 1054-03also shows evolution compared with other rich clusters at lower redshifts, butthe trend is less conclusive if the mass selection effect is considered. Anonnegligible fraction (13%) of cluster members, are forming stars actively andthe overdensity of IR galaxies is about 20 compared to the field. It isunlikely that clusters only passively accrete star forming galaxies from thesurrounding fields and have their star formation quenched quickly afterward;instead, many cluster galaxies still have large amounts of gas, and their starformation may be enhanced by the interaction with the cluster.

IR observations of MS 1054-03: Star Formation and its Evolution in Rich Galaxy Clusters