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A rare opportunity to distinguish internal and environmental effects ongalaxy evolution is afforded by "Supergroups", systems which are rich andmassive but include several comparably rich substructures, surrounded byfilaments. We present here a multiwavelength photometric and spectroscopicstudy of the galaxy population in the Supergroup Abell 1882 at $z$=0.139,combining new data from the MMT and Hectospec with archival results from theGalaxy And Mass Assembly (GAMA) survey, the Sloan Digital Sky Survey (SDSS),NED, the Gemini Multi-Object Spectrograph (GMOS) and Galaxy Evolution Explorer(GALEX). These provide spectroscopic classifications for 526 member galaxies,across wide ranges of local density and velocity dispersion. We identify threeprominent filaments along which galaxies seem to be entering the Supergroup(mostly in E-W directions). Abell 1882 has a well-populated red sequence,containing most galaxies with stellar mass $>$ $10^{10.5}$ $M_{sun}$, and apronounced color-density relation even within its substructures. Thus, galaxyevolution responds to the external environment as strongly in these unrelaxedsystems as we find in rich and relaxed clusters. From these data, local densityremains the primary factor with a secondary role for distance from the inferredcenter of the entire structure's potential well. Effects on star formation, astraced by optical and near-UV colors, depend on galaxy mass. We see changes inlower-mass galaxies (M $<$ $10^{10.5}$ $M_{sun}$) at four times the virialradius of major substructures, while the more massive $NUV$ Green Valleygalaxies show low levels of star formation within two virial radii. Suppressionof star formation ("quenching") occurs in the infall regions of thesestructures even before galaxies enter the denser group environment.

Pre-processing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at $z$=0.139