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We determine the galaxy infrared (IR) luminosity function (LF) as a functionof the environment in a supercluster at z=0.23, using optical, near-IR, andmid- to far-IR photometry, as well as redshifts from optical spectroscopy. Weidentify 467 supercluster members in a sample of 24-micron-selected galaxies,on the basis of their spectroscopic (153) and photometric (314) redshifts. IRluminosities, stellar masses and star formation rates (SFRs) are determined forsupercluster members via spectral energy distribution fitting and the Kennicuttrelation. Galaxies with active galactic nuclei are excluded from the sample. Wedetermine the IR LF of the whole supercluster as well as the IR LFs of threedifferent regions in the supercluster: the cluster core, a large-scalefilament, and the cluster outskirts (excluding the filament). The IR LF showsan environmental dependence which is not simply related to the local galaxydensity. The filament, an intermediate-density region in the A1763supercluster, contains the highest fraction of IR-emitting galaxies at alllevels of IR luminosities. As expected, the core contains the lowest fractionof IR-emitting galaxies and almost no Luminous IR Galaxies (LIRGs). Therelation between galaxy specific SFRs and stellar masses does not depend on theenvironment, and it indicates that most supercluster LIRGs (in particular thosein the filament) are rather massive galaxies with relatively low specific SFRs.A comparison with previous IR LF determinations from the literature confirmsthat the mass-normalized total SFR in clusters increases with redshift, butmore rapidly than previously suggested for redshifts <0.4. We interpret ourfindings within a possible scenario for the evolution of galaxies in and aroundclusters [Abridged].

SPITZER observations of Abell 1763. III. The infrared luminosity function in different supercluster environments