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We present MIPS observations of the cluster A3266. About 100 spectroscopiccluster members have been detected at 24 micron. The IR luminosity function inA3266 is very similar to that in the Coma cluster down to the detection limitL_IR~10^43 ergs/s, suggesting a universal form of the bright end IR LF forlocal rich clusters with M~10^15 M_sun. The shape of the bright end of theA3266-Coma composite IR LF is not significantly different from that of nearbyfield galaxies, but the fraction of IR-bright galaxies (SFR > 0.2M_sun/yr) inboth clusters increases with cluster-centric radius. The decrease of the bluegalaxy fraction toward the high density cores only accounts for part of thetrend; the fraction of red galaxies with moderate SFRs (0.2 < SFR < 1 M_sun/yr)also decreases with increasing galaxy density. These results suggest that forthe IR bright galaxies, nearby rich clusters are distinguished from the fieldby a lower star-forming galaxy fraction, but not by a change in L*_IR. Thecomposite IR LF of Coma and A3266 shows strong evolution when compared with thecomposite IR LF of two z~0.8 clusters, MS 1054 and RX J0152, with L*_IR \propto(1+z)^{3.2+/-0.7},Phi*_IR \propto (1+z)^{1.7+/-1.0}. This L*_IR evolution isindistinguishable from that in the field, and the Phi*_IR evolution isstronger, but still consistent with that in the field. The similarity of theevolution of bright-end IR LF in very different cluster and field environmentssuggests either this evolution is driven by the mechanism that works in bothenvironments, or clusters continually replenish their star-forming galaxiesfrom the field, yielding an evolution in the IR LF that is similar to thefield. The mass-normalized integrated star formation rates (SFRs) of clusterswithin 0.5R_200 also evolve strongly with redshift, as (1+z)^5.3.

The IR Luminosity Functions of Rich Clusters