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The characterization of the internal structure of the superclusters ofgalaxies (walls, filaments and knots where the clusters are located) isparamount for understanding the formation of the Large Scale Structure and foroutlining the environment where galaxies evolved in the last Gyr. (i) To detectthe compact regions of high relative density (clusters and rich groups ofgalaxies); (ii) to map the elongated structures of low relative density(filaments, bridges and tendrils of galaxies); (iii) to characterize the galaxypopulations on filaments and study the environmental effects they are subjectto. We employed optical galaxies with spectroscopic redshifts from theSDSS-DR13 inside rectangular boxes encompassing the volumes of a sample of 46superclusters of galaxies, up to z=0.15. Our methodology implements differentclassical pattern recognition and machine learning techniques pipelined in theGalaxy Systems-Finding algorithm and the Galaxy Filaments-Finding algorithm. Wedetected in total 2,705 galaxy systems (clusters and groups, of which 159 arenew) and 144 galaxy filaments in the 46 superclusters of galaxies. Thefilaments we detected have a density contrast above 3, with a mean value around10, a radius of about 2.5 Mpc and lengths between 9 and 130 Mpc. Correlationsbetween the galaxy properties (mass, morphology and activity) and theenvironment in which they reside (systems, filaments and the dispersedcomponent) suggest that galaxies closer to the skeleton of the filaments aremore massive by up to 25% compared to those in the dispersed component; 70 % ofthe galaxies in the filament region present early type morphologies and thefractions of active galaxies (both AGN and SF) seem to decrease as galaxiesapproach the filament. These results suggest that preprocessing in large scalefilaments could have significant effects on galaxy evolution.

Identification of filamentary structures in the environment of superclusters of galaxies in the Local Universe